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March-April 2024: The Next Full Moon is the Crow, Crust, Sap, Sugar, or Worm Moon


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March-April 2024: The Next Full Moon is the Crow, Crust, Sap, Sugar, or Worm Moon

A full moon rises above snow-capped mountain peaks in this chilly image.
A full moon rises over Utah.
Credits:
NASA/Bill Dunford

The next full moon is the Crow, Crust, Sap, Sugar, or Worm Moon; the Paschal Moon; Purim; the Holi Festival Moon; Madin Poya; the Pothole Moon; a Micromoon, and a Partial Lunar Eclipse.

The next full moon will be on Monday morning, March 25, 2024, appearing opposite the Sun in Earth-based longitude at 3 AM EDT. This will be on Sunday evening from Alaska Time westward to the International Date Line. Around this time the Moon will pass through the partial shadow of the Earth (called a penumbral lunar eclipse). The slight dimming of the Moon will be difficult to notice, but see if you can tell if the lower part of the Moon is dimmer than the upper part. The Moon will begin entering the Earth’s shadow at 12:53 AM, reach greatest eclipse at 3:13 AM with 96% of the Moon in partial shadow, and exit the shadow at 5:32 AM. Since this full Moon is a little over a day after apogee (when the Moon is at its farthest from the Earth in its orbit) this is a micromoon, the opposite of a supermoon. The Moon will appear full for about 3 days around this time, from Saturday evening through Tuesday morning.

The Maine Farmers’ Almanac began publishing “Indian” names for full Moons in the 1930s and these names are now widely known and used. According to this almanac, as the full Moon in March the tribes of the northeastern United States called this the Crow, Crust, Sap, Sugar, or Worm Moon. The more northern tribes of the northeastern States knew this as the Crow Moon, with the cawing of crows signaling the end of winter. Other northern names were the Crust Moon, because the snow cover became crusted from thawing by day and freezing by night, or the Sap (or Sugar) Moon as this was the time for tapping maple trees. The more southern tribes called this the Worm Moon after the earthworm casts that appeared as the ground thawed. It makes sense that only the southern tribes called this the Worm Moon. When glaciers covered the northern part of North America they wiped out the native earthworms. After these glaciers melted about 12,000 years ago the more northern forests grew back without earthworms. Most of the earthworms in these areas are invasive species introduced from Europe and Asia.

In the western Christian ecclesiastical calendar this is the Paschal Moon, from which the date of Easter is calculated. Paschal is the Latinized version of Pesach, Hebrew for Passover. Initially, the Christian holiday of Easter, also called Pascha, was celebrated on the first Sunday after the first full Moon of spring. However, there are differences between the times of these astronomical events and the calendars now used by the Eastern and Western churches. Western Christianity will be celebrating Easter on Sunday, March 31, 2024, the Sunday after this first full Moon of spring. The date of Eastern Orthodox Easter is based on the Julian calendar and will be on Sunday, May 5.

Many lunar and lunisolar calendars start the months on the new Moon with the full Moon in the middle of the month. Lunisolar calendars add or repeat a month as needed to keep the lunar months aligned with the solar seasons. This full Moon is in the middle of the second month of Adar in the Hebrew calendar and corresponds with Purim, celebrated from sunset on March 23 to sunset on March 24, 2024, the 14th of the Adar II (a day later in Jerusalem and ancient walled cities). Purim marks the Jewish people’s deliverance from a royal death decree around the fourth century BCE as told in the Book of Esther. Purim is celebrated by exchanging gifts of food and drink, feasting, and donating to charity.

In the Islamic calendar this full Moon is near the middle of the holy month of Ramadan. Ramadan is honored as the month in which the Quran was revealed. Observing this annual month of charitable acts, prayer, and fasting from dawn to sunset is one of the Five Pillars of Islam.

As the full Moon in the Hindu month Phalguna, this Moon corresponds with the Holi festival, celebrating the victory of good over evil and the start of spring. This two-day long festival is also known as the Festival of Love, Festival of Colors, or the Festival of Spring. Holi begins with a bonfire the evening before the day of the full Moon, continues on the day of the full Moon with a free-for-all game involving the spraying of colored powders and/or colored water on whomever wanders by, and ends with evening visits with friends and family.

Every full Moon is a holiday in Sri Lanka. This full Moon is Medin or Madin Poya, marking the Buddha’s first visit to his father after his enlightenment.

Continuing the tradition of naming Moons after prominent phenomena tied to the time of year, a few years ago my friend Tom Van Wagner suggested naming this the Pothole Moon. It may be a case of confirmation bias, but whether in my car or on my bicycle I notice more potholes this time of year.

As usual, the wearing of suitably celebratory celestial attire is encouraged in honor of the full Moon.

As for other celestial events between now and the full Moon after next (with specific times and angles based on the location of NASA Headquarters in Washington, DC):

Total Eclipse of the Sun

There will be a total eclipse of the Sun on Monday, April 8, 2024. This total eclipse will be visible in a swath ranging from 142 (88 miles) wide near the start and end to 203 km (126 miles) wide near the middle of the swath. The path of the total eclipse will begin in the Pacific south of the equator, start passing over North America on the coast of Mexico near Mazatlán, cross the USA from Texas to Maine, exit North America from Canada on the coast of Newfoundland, and end in the North Atlantic. Outside of this narrow swath, most of North and Central America will see a partial solar eclipse. See https://science.nasa.gov/solar-system/skywatching/eclipses/solar-eclipses/2024-solar-eclipse/total-solar-eclipse-2024-the-moons-moment-in-the-sun/ for more information.

Assuming you can find a place with clear skies near the centerline of this swath, this eclipse, in particular, should be quite a show. Compared to the eclipse in 2017, the Moon will be nearer its closest to the Earth, making its shadow larger, the sky darker, and the eclipse longer. In addition, the Sun will be nearer its maximum in its 11-year cycle, so the corona, which can only be seen during a total eclipse, should be more spectacular. If the sky is clear during the eclipse, you will be able to see the planets and some stars that are not normally visible this time of year. Bright Jupiter will be to the upper left of the eclipse, with Venus, Saturn, and Mars to the lower right. In the unlikely event that the comet 12P/Pons-Brooks has an outburst that makes it significantly brighter (described below), you may be able to see it to the right of Jupiter (if it isn’t obvious, I recommend enjoying the eclipse rather than spending time searching for a comet you might not be able to see).

Plenty of information about this total eclipse is available elsewhere, so I will refrain from adding much more, but please read and pay attention to eye safety. The only time it is safe to look directly at the Sun is when it is completely blocked by the Moon, so that you can only see the much fainter corona. Staring directly at even a small sliver of the Sun can do permanent eye damage.

This eclipse will be passing through or near many populated areas, making it possible to trade off waiting for more accurate weather forecasts for clear skies against the difficulties of making last minute bookings or dealing with  traffic jams if you wait until the day of the eclipse to drive to the zone of totality.

Total eclipses of the Sun are rare and spectacular events. I recognize that not everyone will be able to drop everything and go see this one, but seeing at least one good, total eclipse in a clear sky should be on your bucket list. A partial eclipse is just not the same. The only other reason I can think of for not going where you can see this total eclipse (other than you absolutely can’t at this time) is that if you see this eclipse, you are likely to want to see more, and will begin making plans to go to North Africa in 2026, Australia in 2028, etc. The next three eclipses visible from parts of North America will be in 2044, 2045, and 2052.

Comet 12P/Pons-Brooks

During this lunar cycle, comet 12P/Pons-Brooks will be visible with binoculars or a telescope, and may become bright enough to be a naked eye comet. In my quick searches of the web I found visual guides that provide specific information on when and where to look from your location on any given night. However, I did not see a concise guide to when might be the best time to look for this comet, so here is my meager attempt.

Several things make a difference in how easy it is to see a comet.

The greatest uncertainty is how much dust and gas it will be giving off, as it is the sunlight illuminating these plumes that make the comet bright. This comet has already had outbursts that have made it temporarily 10 to 100 times brighter. It may be less likely such outbursts will occur as the comet moves closer to the Sun, but this is uncertain. As the astronomer David H. Levy said, “Comets are like cats; they have tails, and they do precisely what they want.”

My recommendation is to pay attention to the news and check regularly to see if the comet has had an outburst, as this may push its brightness into the visible range. In addition, I plan to look for the comet with binoculars, both on April 8 and 9 before moonlight begins to interfere and in the weeks before closest approach to the Sun on April 21. The next couple of paragraphs give my reasoning (which you are welcome to skip if you like).

We can’t predict outbursts, but we can predict other influences on the brightness of the comet.

If the gas and dust from the comet isn’t changing, an easy calculation is to assume the comet will scatter light uniformly in all directions, so that all you need to consider is the distance between the Sun and the comet and the distance between the comet and the Earth. This suggests that the comet will be at its brightest around April 20 and 21, 2024, when it will be passing its closest to the Sun and receiving (and reflecting towards Earth) the maximum amount of sunlight.

How easy the comet will be to see will also depend on how much glow there is from twilight (which depends on how far the Sun is below the horizon), whether (and how much) moonlight there is (increased moonlight will brighten the background sky), and how high the comet is above the horizon.

In the evenings, nautical twilight ends when the Sun reaches 12 degrees below the horizon (the estimate of when the horizon will be too dark for sailors at sea to use for navigation). In mid-to-late April (for the DC area), nautical twilight ends about 1 hour after sunset (the start and end of twilight I use throughout these Moon Missives is based on nautical twilight). Astronomical twilight is when the Sun is between 12 and 18 degrees below the horizon, when the sky looks dark but there can be enough residual glow that the faintest stars and diffuse objects (like nebulae, galaxies, faint meteors, and comets on the edge of visibility) may be masked. When the Sun is more than 18 degrees below the horizon the sky is about as dark as it is going to get.

When the Moon is in the sky it will add its light to the background brightness of the sky. The amount of light added will increase as the Moon waxes from a faint, thin crescent to a bright, nearly full Moon.

The evening of April 8, 2024, as nautical twilight ends (at 8:39 PM EDT), the crescent Moon will have already set and the comet will be 11.4 degrees above the west-northwestern horizon. The combined effect of the range from the Sun and the Earth gives a geometric estimate of 91% of the maximum brightness at its closest to the Sun in late April. By the time astronomical twilight ends (at 9:12 PM) the comet will still be 5 degrees above the horizon.

The evening of April 9, it might be interesting to see the comet and the thin, waxing crescent Moon low on the horizon as twilight ends, as the Moon will not be very bright and should not interfere much with seeing the comet. Nautical twilight will end (at 8:40 PM) with the Moon 4.2 degrees above the horizon and the comet above the Moon at 10.8 degrees above the horizon. The Moon will set (at 9:08 PM) just 5 minutes before astronomical twilight ends (at 9:13 PM), when the comet will be 4.6 degrees above the horizon. The distance-based estimate of brightness will have increased to 93% of the peak in late April.

Between April 10 and April 21, the geometric estimate of the brightness of the comet will gradually increase, but so will interference from the brightness of the waxing Moon, and the comet will shift closer to the horizon each evening. On the evening of April 21 the geometric brightness of the comet will be at its greatest, but the Moon will be 96% illuminated and the comet will be only 2.7 degrees above the horizon as nautical twilight ends. April 24 will be the last evening that the comet will be above the horizon before nautical twilight ends (at 8:57 PM).

Note that as our opportunity to view this comet from northern latitudes gets worse in late April, the opportunity for viewers in the Southern Hemisphere will get better.

Length of Daylight

As spring continues the daily periods of sunlight continue to lengthen, having changed at their fastest around the equinox on March 19, 2024. On Monday, March 25 (the day of the full Moon), morning twilight will begin at 6:05 AM, sunrise will be at 7:03 AM, solar noon will be at 1:14 PM when the Sun will reach its maximum altitude of 53.3 degrees, sunset will be at 7:25 PM, and evening twilight will end at 8:24 PM. By Tuesday, April 23 (the day of the full Moon after next), morning twilight will begin at 5:18 AM, sunrise will be at 6:20 AM, solar noon will be at 1:06 PM when the Sun will reach its maximum altitude of 64.0 degrees, sunset will be at 7:53 PM, and evening twilight will end at 8:56 PM.

Meteor Showers

Two meteor showers, the Lyrids (006 LYR) and the π-Puppids (137 PPU), will peak near the end of this lunar cycle but the nearly full Moon will interfere with seeing these meteors.

Evening Sky Highlights

On the evening of Sunday, March 24 (the evening before the full Moon), as twilight ends (at 8:22 PM EDT), the rising Moon will be 14 degrees above the east-southeastern horizon. The bright planet Jupiter will be 27 degrees above the western horizon and the planet Mercury will be to the lower right of Jupiter at 7 degrees above the horizon. The bright object appearing closest to overhead will be Pollux at 78 degrees above the south-southeastern horizon. Pollux is the 17th brightest star in our night sky and the brighter of the twin stars in the constellation Gemini the twins. Pollux is an orange tinted star about 34 light-years from Earth. It is not quite twice the mass of our Sun but about 9 times the diameter and 33 times the brightness.

As this lunar cycle progresses, the background of stars will appear to shift westward each evening (as the Earth moves around the Sun). Mercury will be dimming as it shifts toward the west-northwestern horizon, with April 3 the last evening it will be above the horizon as twilight ends and April 11 when it will pass between the Earth and the Sun, shifting from the evening to the morning sky. We are approaching the end of the opportunity to view Jupiter for this apparition, as it will shift lower towards the west-northwestern horizon each evening. The waxing Moon will pass by Jupiter on April 10, Pollux on April 14 and 15, Regulus on April 17 and 18, and Spica on April 22. By the evening of Tuesday, April 23 (the evening of the day of the full Moon after next), as twilight ends (at 8:56 PM EDT), the rising Moon will be 10 degrees above the east-southeastern horizon. The bright planet Jupiter will be 4 degrees above the west-northwestern horizon. The bright object appearing closest to overhead will be Regulus at 63 degrees above the southern horizon. Regulus is the 21st brightest star in our night sky and the brightest star in the constellation Leo the lion. The Arabic name for Regulus translates as “the heart of the lion.” Although we see Regulus as a single star, it is actually four stars (two pairs of stars orbiting each other). Regulus is about 79 light-years from us.

Morning Sky Highlights

On the morning of Monday, March 25 (the morning after the full Moon), as twilight begins (at 6:05 AM EDT), the setting Moon will be 12 degrees above the west-southwestern horizon. The planet Mars will be 3 degrees above the east-southeastern horizon. The bright object appearing closest to overhead will be the star Vega at 73 degrees above the eastern horizon. Vega is the brightest star in the constellation Lyra the lyre and is one of the three bright stars in the “Summer Triangle” along with Deneb and Altair. Vega is the 5th brightest star in our night sky, about 25 light-years from Earth, twice the mass of our Sun, and shines 40 times brighter than our Sun.

As this lunar cycle progresses, the background of stars will appear to shift westward each evening, while Mars will hover low on the east-southeastern horizon, drifting slightly to the left. The waning Moon will pass by Spica on March 26 and 27, and Antares on March 30. April 1 will be the first morning the planet Saturn will be above the eastern horizon as morning twilight begins, shifting towards Mars each morning. On April 6 the thin, waning crescent Moon will form a triangle with Saturn and Mars, but will be low on the east-southeastern horizon and difficult to see, with the Moon rising just 3 minutes before morning twilight begins. On April 10 Mars and Saturn will appear closest to each other, after which they will appear to separate. By the morning of Tuesday, April 23 (the morning of the day of the full Moon after next), as twilight begins (at 5:18 AM EDT), the setting full Moon will be 7 degrees above the west-southwestern horizon with the bright star Spica 2.5 degrees to the lower left of the Moon. The planet Mars will be 5 degrees above the eastern horizon and the planet Saturn will be 7 degrees above the east-southeastern horizon. The bright object appearing closest to overhead will still be the star Vega at 86 degrees above the eastern horizon.

Detailed Daily Guide

Here for your reference is a day-by-day listing of celestial events between now and the full Moon after next. The times and angles are based on the location of NASA Headquarters in Washington, DC, and some of these details may differ for where you are (I use parentheses to indicate times specific to the DC area).

Monday evening into Tuesday morning, March 18 to 19, 2024, the bright star Pollux (the brighter of the twin stars in the constellation Gemini the twins) will appear near the waxing gibbous Moon. Pollux will be 3.5 degrees to the left as twilight ends (at 8:16 PM EDT) and will shift clockwise around the Moon until the Moon sets on the northwestern horizon (at 4:42 AM) when Pollux will be 2 degrees to the upper right.

Tuesday evening, March 19, 2024, at 11:06 PM EDT, will be the vernal equinox, the astronomical end of winter and start of spring. For a location on the equator in the ocean north of Western New Guinea the Sun will pass directly overhead as it shifts from the Southern to the Northern Hemisphere.

Thursday morning, March 21, 2024, if you have a very clear view of the horizon about halfway between east and east-southeast, you might be able to see the planet Saturn less than a degree to the lower left of the bright planet Venus. Because of the glow of dawn this will be hard to see. Venus will shine brighter than any star, but Saturn will rise last (at 6:32 AM), 21 minutes after twilight begins (at 6:11 AM EDT), and will be only a little brighter than the star Pollux, the 17th brightest star in our night sky. You may need binoculars to see the pair, but make sure you stop looking well before sunrise.

The next morning, Friday, March 22, 2024, the planet Venus will have shifted to less than a degree to the left of the planet Saturn, with the pair rising together (at 6:29 AM EDT) 19 minutes after twilight begins (at 6:10 AM).

Thursday evening into Friday morning, March 21 to 22, 2024, the bright star Regulus will appear near the waxing gibbous Moon. As twilight ends (at 8:19 PM EDT) Regulus will be 5 degrees to the lower right of the Moon. Regulus will gradually shift closer to the Moon, initially swinging towards the left (appearing 4 degrees below and a little to the left) as the Moon reaches its highest (at 11:13 PM). At about 2:30 AM (when Regulus will be 3 degrees to the lower left) Regulus will switch and start swinging towards the right. As Regulus sets (at 5:58 AM) it will be 2.5 degrees below the Moon, with morning twilight beginning 12 minutes later (at 6:10 AM) and the Moon setting 3 minutes after that (at 6:13 AM).

Saturday night, March 23, 2024, at 11:46 AM EDT, the Moon will be at apogee, its farthest from the Earth for this orbit.

Sunday evening, March 24, 2024, at 5:59 PM EDT, will be when the planet Mercury reaches its greatest angular separation from the Sun as seen from Earth for this apparition (called greatest elongation). This will be the evening when the planet Mercury will appear highest above the western horizon (6.5 degrees) as twilight ends (at 8:22 PM).

As mentioned above, the next full Moon will be on Monday morning, March 25, 2024. The Moon will pass through the partial shadow of the Earth (called a penumbral lunar eclipse), beginning to enter the shadow at 12:53 AM EDT, reaching greatest eclipse at 3:13 AM when 96% of the Moon will be in partial shadow, and exiting the shadow at 5:32 AM. The slight dimming of the Moon will be difficult to notice. Since this is a little over a day after apogee (when the Moon is at its farthest from the Earth in its orbit) this will be a micromoon, the opposite of a supermoon. The Moon will appear full for about 3 days around this time, from Saturday evening through Tuesday morning.

Tuesday morning, March 26, 2024, the bright star Spica will appear near the full Moon. As the Moon reaches its highest in the sky for the night (at 1:52 AM EDT), Spica will be 8 degrees to the lower left of the Moon. By the time twilight begins (at 6:03 AM), Spica will be 6 degrees to the left of the Moon.

Tuesday evening into Wednesday morning, March 26 to 27, 2024, the Moon will have shifted to the other side of Spica. As the Moon rises on the east-southeastern horizon (at 8:59 PM EDT), Spica will be 3 degrees to the upper right of the Moon. By the time the Moon reaches its highest for the night (at 2:32 AM), Spica will be 5 degrees to the upper right. Spica will be 6 degrees to the lower right as twilight begins (at 6:02 AM).

Saturday morning, March 30, 2024, the bright star Antares will appear near the waning gibbous Moon. As Antares rises on the southeastern horizon (at 12:37 AM EDT) it will be 5 degrees to the lower left of the Moon. The Moon will reach its highest for the night (at 4:52 AM) with Antares 3 degrees to the left. As twilight begins (at 5:57 AM) Antares will be a little less than 3 degrees to the upper left of the Moon.

Monday morning, April 1, 2024, will be the first morning that the planet Saturn will be above the eastern horizon as twilight begins (at 5:55 AM EDT).

Monday night, April 1, 2024, the waning Moon will appear half-full as it reaches its last quarter at 11:15 PM EDT (when the Moon will be below the horizon).

Wednesday evening, April 3, 2024, will be the last evening that the planet Mercury will be above the horizon as twilight ends.

Saturday morning, April 6, 2024, if you have a very clear view of the east-southeastern horizon, you might be able to see the thin, waning crescent Moon near the planets Saturn and Mars. The Moon will rise last (at 5:42 AM EDT) just 3 minutes before twilight begins, with

Saturn 2 degrees to the upper left of the Moon and Mars 4 degrees to the upper right of the Moon.

You will need binoculars to see them in the glow of dawn, but on Sunday morning, April 7, 2024, the bright planet Venus will appear 3.5 degrees to the left of the very thin, waning crescent Moon low on the eastern horizon. Venus will rise last (at 6:14 AM EDT) 31 minutes after twilight begins and 29 minutes before sunrise. If you are using binoculars to scan for this pairing, be sure to stop looking well before any chance of sunrise (as using high powered lenses to focus intense sunlight directly into your eyes is a really bad idea).

Sunday afternoon, April 7, 2024, at 1:52 PM EDT, the Moon will be at perigee, its closest to the Earth for this orbit.

There will be an eclipse of the Sun on Monday, April 8, 2024. For information on the total solar eclipse (not visible from the Washington, DC area) see the summary section above. The Washington, DC area will only see a partial eclipse, starting at about 2:04 PM EDT, reaching its peak at about 3:21 PM when 88.9% of the Sun will be blocked by the Moon, and ending at 4:33 PM. Please pay attention to eye safety and do not look at the Sun directly without eclipse glasses. When the Moon is blocking most of the Sun, what remains will appear like a crescent. One of the interesting effects is that the sunlight through trees, etc., that we normally see as mottled sunlight (round blotches of light) is actually made up of many small images of the round Sun. When the Sun appears as a crescent these mottled patches will appear as many small crescents.

The eclipse will also be the new Moon, when the Moon passes between the Earth and the Sun and is not usually visible from the Earth (except when its silhouette causes an eclipse). The day of or the day after the new Moon marks the start of the new month for most lunisolar calendars. Sundown on Monday, April 8, 2024, marks the start of Nisan in the Hebrew calendar. Pesach or Passover begins on the 15th day of Nisan. The third month of the Chinese calendar starts on Tuesday, April 9, 2023.

Monday evening, April 8, 2024, as nautical or evening twilight ends (at 8:39 PM EDT), comet 12P/Pons-Brooks will be 11.4 degrees above the west-northwestern horizon. The crescent Moon will have already set, making this the last evening to see this comet without moonlight. By the time astronomical twilight ends (at 9:12 PM) the comet will still be 5 degrees above the horizon.

In the Islamic calendar the months traditionally start with the first sighting of the waxing crescent Moon. Many Muslim communities now follow the Umm al-Qura Calendar of Saudi Arabia, which uses astronomical calculations to start months in a more predictable way. This calendar predicts the holy month of Ramadan will end and Shawwāl will begin with sunset on Tuesday, April 9, 2024. Because of the religious significance of the end of Ramadan, Shawwāl is one of 4 months in the Islamic year where the start of the month is updated in the Umm al-Qura Calendar based upon the actual sighting of the crescent Moon. Starting with the sighting of the crescent Moon, the end of the Ramadan fast will be celebrated with Eid al-Fitr (the Feast of Breaking the Fast), a celebration lasting from 1 to 3 days.

Tuesday evening, April 9, 2024, it should be interesting to see the comet 12P/Pons-Brooks and the thin, waxing crescent Moon low on the horizon as twilight ends, as the Moon will not be very bright and should not interfere much with seeing the comet. Nautical or evening twilight will end (at 8:40 PM EDT) with the Moon 4.2 degrees above the horizon and the comet above the Moon at 10.8 degrees above the horizon. The Moon will set (at 9:08 PM) just 5 minutes before astronomical twilight ends (at 9:13 PM), when the comet will be 4.6 degrees above the horizon.

In the mornings throughout this lunar cycle the planets Saturn and Mars will appear near each other low on the east-southeastern horizon. Both will appear to shift higher each morning, with Saturn shifting more than Mars. Wednesday morning, April 10, 2024, will be when the pair will be at their closest. As twilight begins (at 5:38 AM EDT) the slightly brighter Saturn will appear 3 degrees above the horizon with Mars 0.5 degrees above Saturn.

Wednesday evening, April 10, 2024, the bright planet Jupiter will appear 4 degrees to the lower left of the waxing crescent Moon. The Moon will be 17 degrees above the west-northwestern horizon as twilight ends (at 8:41 PM EDT) and Jupiter will set first 77 minutes later (at 9:58 PM).

Thursday evening, April 11, 2024, the Pleiades star cluster will appear 6 degrees to the lower right of the waxing crescent Moon. The Moon will be 30 degrees above the western horizon as twilight ends (at 8:42 PM EDT) and the Pleiades will set first a little over 2 hours later (at about 11 PM).

Thursday evening, April 11, 2024, the planet Mercury will be passing between the Earth and the Sun, called inferior conjunction. Planets that orbit inside of the orbit of Earth can have two types of conjunctions with the Sun, inferior (when passing between the Earth and the Sun) and superior (when passing on the far side of the Sun). Mercury will be shifting from the evening sky to the morning sky and will begin emerging from the glow of the dawn on the eastern horizon later in April (depending upon viewing conditions).

Sunday evening into early Monday morning, April 14 to 15, 2024, the bright star Pollux (the brighter of the twins in the constellation Gemini the twins) will appear to the upper left of the waxing crescent Moon. As twilight ends (at 8:45 PM EDT) Pollux will be 8 degrees from the Moon. By the time the Moon sets on the west-northwestern horizon (at 2:39 AM), Pollux will be 5 degrees from the Moon.

Monday afternoon, April 15, 2024, the Moon will appear half-full as it reaches its first quarter at 3:13 PM EDT (when it will be daylight with the Moon visible in the eastern sky).

Monday evening into early Tuesday morning, April 15 to 16, 2024, the half-Moon will have shifted such that the bright star Pollux will appear to the lower right of the Moon. As twilight ends (at 8:45 PM EDT) Pollux will be 6 degrees from the Moon and the pair will appear to separate as the night progresses, reaching 8 degrees apart around 1:30 AM.

Wednesday evening into Thursday morning, April 17 to 18, 2024, the bright star Regulus will appear to the lower left of the waxing gibbous Moon. As twilight ends (at 8:49 PM EDT) Regulus will be 7.5 degrees from the Moon. When Regulus sets on the west-northwestern horizon (at 4:12 AM) it will be 4.5 degrees from the Moon.

Thursday evening into Friday morning, April 18 to 19, 2024, the waxing gibbous Moon will have shifted to the other side of the bright star Regulus. As twilight ends (at 8:50 PM EDT) Regulus will be 6 degrees to the upper right of the Moon. About 1 hour later (at 9:53 PM) the Moon will reach its highest for the night with Regulus 6 degrees to the right. Regulus will appear to rotate clockwise around and to separate from the Moon as the night progresses, reaching about 8 degrees to the lower right around 3 AM.

Friday night, April 19, 2024, at 10:09 PM EDT, the Moon will be at apogee, its farthest from the Earth for this orbit.

Friday morning, April 19, 2024, will be the first morning that the planet Mercury will rise more than 30 minutes before sunrise, a very rough estimate of the earliest it might start being visible in the glow of dawn on the eastern horizon. Mercury will be quite faint, but will brighten each morning as it presents a larger illuminated crescent towards the Earth. However, this will not be a favorable apparition for Mercury viewing, as even at its highest it will not rise before twilight begins.

Sunday, April 21, 2024 will be when the comet 12P/Pons-Brooks will be at its closest to the Sun, and the week or two before this might be a good time to look for this comet with binoculars. If the trail of gas and dust the comet is giving off doesn’t change significantly (a very big and uncertain “if”) then the brightness of the comet should gradually increase to a maximum on April 21. However, interference from the light of the waxing Moon will also increase beginning April 9, and the comet will shift closer to the horizon each evening. As twilight ends on April 21 (at 8:53 PM EDT) the Moon will be 96% illuminated and the comet will be only 2.7 degrees above the horizon. April 24 will be the last evening that the comet will be above the horizon before evening twilight ends (at 8:57 PM).

Monday evening into Tuesday morning, April 22 to 23, 2024, the bright star Spica will appear to the lower right of the full Moon. Spica will be a little more than 1 degree from the Moon as twilight ends. They will be at their closest a little before midnight. Spica will be 1 degree from the Moon as the Moon reaches its highest for the night (at 12:31 AM) and will be 2.5 degrees from the Moon as twilight begins (at 5:18 AM).

The full Moon after next will be Tuesday evening, April 23, 2024, at 7:49 PM EDT. This will be on Wednesday from the UK, Ireland, and Portugal eastward across Europe, Africa, Asia, and Australia to the International Date Line in the mid-Pacific. The Moon will appear full for about 3 days centered on this time, from Monday morning to Thursday morning.

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    • By NASA
      1 min read
      Preparations for Next Moonwalk Simulations Underway (and Underwater)
      Dr. Misty Davies receives the prestigious AIAA Fellowship in May 2024 for her contributions to aerospace safety and autonomous systems, recognized at a ceremony in Washington, DC.NASA In May 2024, Dr. Misty Davies joined the American Institute of Aeronautics and Astronautics (AIAA) Class of 2024 Fellows at a ceremony in Washington, DC.  The AIAA website states that, “AIAA confers Fellow upon individuals in recognition of their notable and valuable contributions to the arts, sciences or technology of aeronautics and astronautics.”  The first AIAA Fellows were elected in 1934; since then only 2064 people have been selected for the honor.  Dr. Davies has focused her career at NASA Ames Research Center on developing tools and techniques that enable the safety assurance of increasingly autonomous systems.  She currently serves as the Associate Chief for Aeronautics Systems in the Intelligent Systems Division at NASA Ames and is the Aerospace Operations and Safety Program (AOSP) Technical Advisor for Assurance and Safety. More information on AIAA Fellows is at https://www.aiaa.org/news/news/2024/02/08/aiaa-announces-class-of-2024-honorary-fellows-and-fellows
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      Last Updated Nov 22, 2024 Related Terms
      General Explore More
      8 min read SARP East 2024 Ocean Remote Sensing Group
      Article 52 mins ago 10 min read SARP East 2024 Atmospheric Science Group
      Article 52 mins ago 10 min read SARP East 2024 Hydroecology Group
      Article 52 mins ago Keep Exploring Discover Related Topics
      Missions
      Humans in Space
      Climate Change
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      View the full article
    • By NASA
      8 min read
      Preparations for Next Moonwalk Simulations Underway (and Underwater)
      Return to 2024 SARP Closeout Faculty Advisors:
      Dr. Tom Bell, Woods Hole Oceanographic Institution
      Dr. Kelsey Bisson, NASA Headquarters Science Mission Directorate
      Graduate Mentor:
      Kelby Kramer, Massachusetts Institute of Technology

      Kelby Kramer, Graduate Mentor
      Kelby Kramer, graduate mentor for the 2024 SARP Ocean Remote Sensing group, provides an introduction for each of the group members and shares behind-the scenes moments from the internship.
      Lucas DiSilvestro
      Shallow Water Benthic Cover Type Classification using Hyperspectral Imagery in Kaneohe Bay, Oahu, Hawaii
      Lucas DiSilvestro
      Quantifying the changing structure and extent of benthic coral communities is essential for informing restoration efforts and identifying stressed regions of coral. Accurate classification of shallow-water benthic coral communities requires high spectral and spatial resolution, currently not available on spaceborne sensors, to observe the seafloor through an optically complex seawater column. Here we create a shallow water benthic cover type map of Kaneohe Bay, Oahu, Hawaii using the Airborne Visible/Infrared Imaging Spectrometer (AVIRIS) without requiring in-situ data as inputs. We first run the AVIRIS data through a semi-analytical inversion model to derive color dissolved organic matter, chlorophyll concentration, bottom albedo, suspended sediment, and depth parameters for each pixel, which are then matched to a Hydrolight simulated water column. Pure reflectance for coral, algae, and sand are then projected through each water column to create spectral endmembers for each pixel. Multiple Endmember Spectral Mixture Analysis (MESMA) provides fractional cover of each benthic class on a per-pixel basis. We demonstrate the efficacy of using simulated water columns to create surface reflectance spectral endmembers as Hydrolight-derived in-situ endmember spectra strongly match AVIRIS surface reflectance for corresponding locations (average R = 0.96). This study highlights the capabilities of using medium-fine resolution hyperspectral imagery to identify fractional cover type of localized coral communities and lays the groundwork for future spaceborne hyperspectral monitoring of global coral communities.

      Atticus Cummings
      Quantifying Uncertainty In Kelp Canopy Remote Sensing Using the Harmonized Landsat Sentinel-2 Dataset
      Atticus Cummings
      California’s giant kelp forests serve as a major foundation for the region’s rich marine biodiversity and provide recreational and economic value to the State of California. With the rising frequency of marine heatwaves and extreme weather onset by climate change, it has become increasingly important to study these vital ecosystems. Kelp forests are highly dynamic, changing across several timescales; seasonally due to nutrient concentrations, waves, and predator populations, weekly with typical growth and decay, and hourly with the tides and currents. Previous remote sensing of kelp canopies has relied on Landsat imagery taken with a eight-day interval, limiting the ability to quantify more rapid changes. This project aims to address uncertainty in kelp canopy detection using the Harmonized Landsat and Sentinel-2 (HLS) dataset’s zero to five-day revisit period. A random forest classifier was used to identify pixels that contain kelp, on which Multiple Endmember Spectral Mixture Analysis (MESMA) was then run to quantify intrapixel kelp density. Processed multispectral satellite images taken within 3 days of one another were paired for comparison. The relationship between fluctuations in kelp canopy density with tides and currents was assessed using in situ data from an acoustic doppler current profiler (ADCP) at the Santa Barbara Long Term Ecological Research site (LTER) and a NOAA tidal buoy. Preliminary results show that current and tidal trends cannot be accurately correlated with canopy detection due to other sources of error. We found that under cloud-free conditions, canopy detection between paired images varied on average by 42%. Standardized image processing suggests that this uncertainty is not created within the image processing step, but likely arises due to exterior factors such as sensor signal noise, atmospheric conditions, and sea state. Ultimately, these errors could lead to misinterpretation of remotely sensed kelp ecosystems, highlighting the need for further research to identify and account for uncertainties in remote sensing of kelp canopies.

      Jasmine Sirvent
      Kelp Us!: A Methods Analysis for Predicting Kelp Pigment Concentrations from Hyperspectral Reflectance
      Jasmine Sirvent
      Ocean color remote sensing enables researchers to assess the quantity and physiology of life in the ocean, which is imperative to understanding ecosystem health and formulating accurate predictions. However, without proper methods to analyze hyperspectral data, correlations between spectral reflectance and physiological traits cannot be accurately derived. In this study, I explored different methods—single variable regression, partial least squares regressions (PLSR), and derivatives—in analyzing in situ Macrocystis pyrifera (giant kelp) off the coast of Santa Barbara, California in order to predict pigment concentrations from AVIRIS hyperspectral reflectance. With derivatives as a spectral diagnostic tool, there is evidence suggesting high versus low pigment concentrations could be diagnosed; however, the fluctuations were within 10 nm of resolution, thus AVIRIS would be unable to reliably detect them. Exploring a different method, I plotted in situ pigment measurements — chlorophyll a, fucoxanthin, and the ratio of fucoxanthin to chlorophyll a—against hyperspectral reflectance that was resampled to AVIRIS bands. PLSR proved to be a more successful model because of its hyperdimensional analysis capabilities in accounting for multiple wavelength bands, reaching R2 values of 0.67. Using this information, I constructed a model that predicts kelp pigments from simulated AVIRIS reflectance using a spatial time series of laboratory spectral measurements and photosynthetic pigment concentrations. These results have implications, not only for kelp, but many other photosynthetic organisms detectable by hyperspectral airborne or satellite sensors. With these findings, airborne optical data could possibly predict a plethora of other biogeochemical traits. Potentially, this research would permit scientists to acquire data analogous to in situ measurements about floating matters that cannot financially and pragmatically be accessed by anything other than a remote sensor.

      Isabelle Cobb
      Correlations Between SSHa and Chl-a Concentrations in the Northern South China Sea
      Isabelle Cobb
      Sea surface height anomalies (SSHa)–variations in sea surface height from climatological averages–occur on seasonal timescales due to coastal upwelling and El Niño-Southern Oscillation (ENSO) cycles. These anomalies are heightened when upwelling plumes bring cold, nutrient-rich water to the surface, and are particularly strong along continental shelves in the Northern South China Sea (NSCS). This linkage between SSHa and nutrient availability has interesting implications for changing chlorophyll-a (chl-a) concentrations, a prominent indicator of phytoplankton biomass that is essential to the health of marine ecosystems. Here, we evaluate the long-term (15 years) relationship between SSHa and chl-a, in both satellite remote sensing data and in situ measurements. Level 3 SSHa data from Jason 1/2/3 satellites and chl-a data from MODIS Aqua were acquired and binned to monthly resolution. We found a significant inverse correlation between SSHa and chl-a during upwelling months in both the remote sensing (Spearman’s R=-0.57) and in situ data, with higher resolution in situ data from ORAS4 (an assimilation of buoy observations from 2003-2017) showing stronger correlations (Spearman’s R=-0.75). In addition, the data reveal that the magnitude of SSH increases with time during instances of high correlation, possibly indicating a trend of increased SSH associated with reduced seasonal chl-a concentrations. Thus, this relationship may inform future work predicting nutrient availability and threats to marine ecosystems as climate change continues to affect coastal sea surface heights.

      Alyssa Tou
      Exploring Coastal Sea Surface Temperature Anomalies and their effect on Coastal Fog through analyzing Plant Phenology
      Alyssa Tou
      Marine heat waves (MHW) have been increasing in frequency, duration and intensity, giving them substantial potential to influence ecosystems. Do these MHWs sufficiently enhance coastal precipitation such that plant growth is impacted? Recently, the Northeast Pacific experienced a long, intense MHW in 2014/2015, and another short, less intense MHW in 2019/2020. Here we investigate how the intensity and duration of MHWs influence the intensity and seasonal cycle of three different land cover types (‘grass’, ‘trees’, and a combination of both ‘combined’’) to analyze plant phenology trends in Big Sur, California. We hypothesize that longer intense MHWs decrease the ocean’s evaporative capacity, decreasing fog, thus lowering plant productivity, as measured by Normalized Difference Vegetation Index (NDVI). Sea surface temperature (SST) and NDVI data were collected from the NOAA Coral Reef Watch, and NASA MODIS/Terra Vegetation Indices 16-Day L3 Global 250m products respectively. Preliminary results show no correlation (R2=0.02) between SSTa and combined NDVI values and no correlation (R2=0.01) between SST and NDVI. This suggests that years with anomalously high SST do not significantly impact plant phenology. During the intense and long 2014/2015 MHW, peak NDVI values for ‘grass’ and ‘combined’ pixels were 2.0 and 1.7 standard deviations above the climatological average, while the shorter 2019/2020 MHW saw higher peaks of 3.2 and 2.4 standard deviations. However, the ‘grass’, ‘tree’ and ‘combined’ NDVI anomalies were statistically insignificant during both MHWs, showing that although NDVI appeared to increase during the shorter and less intense MHW, these values may be attributed to other factors. The data qualitatively suggest that MHW’s don’t impact the peak NDVI date, but more data at higher temporal resolution are necessary. Further research will involve analyzing fog indices and exploring confounding variables impacting NDVI, such as plant physiology, anthropogenic disturbance, and wildfires. In addition, it’s important to understand to what extent changes in NDVI are attributed to the driving factors of MHWs or the MHWs themselves. Ultimately, mechanistically understanding the impacts MHW intensity and duration have on terrestrial ecosystems will better inform coastal community resilience.


      Return to 2024 SARP Closeout Share
      Details
      Last Updated Nov 22, 2024 Related Terms
      General Explore More
      10 min read SARP East 2024 Atmospheric Science Group
      Article 21 mins ago 10 min read SARP East 2024 Hydroecology Group
      Article 21 mins ago 11 min read SARP East 2024 Terrestrial Fluxes Group
      Article 22 mins ago View the full article
    • By NASA
      10 min read
      Preparations for Next Moonwalk Simulations Underway (and Underwater)
      Return to 2024 SARP Closeout Faculty Advisors:
      Dr. Guanyu Huang, Stony Brook University
      Graduate Mentor:
      Ryan Schmedding, McGill University

      Ryan Schmedding, Graduate Mentor
      Ryan Schmedding, graduate mentor for the 2024 SARP Atmospheric Science group, provides an introduction for each of the group members and shares behind-the scenes moments from the internship.
      Danielle Jones
      Remote sensing of poor air quality in mountains: A case study in Kathmandu, Nepal
      Danielle Jones
      Urban activity produces particulate matter in the atmosphere known as aerosol particles. These aerosols can negatively affect human health and cause changes to the climate system. Measures for aerosols include surface level PM2.5 concentration and aerosol optical depth (AOD). Kathmandu, Nepal is an urban area that rests in a valley on the edge of the Himalayas and is home to over three million people. Despite the prevailing easterly winds, local aerosols are mostly concentrated in the valley from the residential burning of coal followed by industry. Exposure to PM2.5 has caused an estimated ≥8.6% of deaths annually in Nepal. We paired NASA satellite AOD and elevation data, model  meteorological data, and local AirNow PM2.5 and air quality index (AQI) data to determine causes of variation in pollutant measurement during 2023, with increased emphasis on the post-monsoon season (Oct. 1 – Dec. 31). We see the seasonality of meteorological data related to PM2.5 and AQI. During periods of low temperature, low wind speed, and high pressure, PM2.5 and AQI data slightly diverge. This may indicate that temperature inversions increase surface level concentrations of aerosols but have little effect on the total air column. The individual measurements of surface pressure, surface temperature, and wind speed had no observable correlation to AOD (which was less variable than PM2.5 and AQI over the entire year). Elevation was found to have no observable effect on AOD during the period of study. Future research should focus on the relative contributions of different pollutants to the AQI to test if little atmospheric mixing causes the formation of low-altitude secondary pollutants in addition to PM2.5 leading to the observed divergence in AQI and PM2.5.

      Madison Holland
      Analyzing the Transport and Impact of June 2023 Canadian Wildfire Smoke on Surface PM2.5 Levels in Allentown, Pennsylvania
      Madison Holland
      The 2023 wildfire season in Canada was unparalleled in its severity. Over 17 million hectares burned, the largest area ever burned in a single season. The smoke from these wildfires spread thousands of kilometers, causing a large population to be exposed to air pollution. Wildfires can release a variety of air pollutants, including fine particulate matter (PM2.5). PM2.5 directly affects human health – exposure to wildfire-related PM2.5 has been associated with respiratory issues such as the exacerbation of asthma and chronic obstructive pulmonary disease. In June 2023, smoke from the Canadian wildfires drifted southward into the United States. The northeastern United States reported unhealthy levels of air quality due to the transportation of the smoke. In particular, Pennsylvania reported that Canadian wildfires caused portions of the state to have “Hazardous” air quality. Our research focused on how Allentown, PA experienced hazardous levels of air quality from this event. To analyze the concentrations of PM2.5 at the surface level, NASA’s Hazardous Air Quality Ensemble System (HAQES) and the EPA’s Air Quality System (AQS) ground-based site data were utilized. By comparing HAQES’s forecast of hazardous air quality events with recorded daily average PM2.5 with the EPA’s AQS, we were able to compare how well the ensemble system was at predicting total PM2.5 during unhealthy air quality days. NOAA’s Hybrid Single-Particle Lagrangian Integrated Trajectory model, pyrsig, and the Canadian National Fire Database were used. These datasets revealed the trajectory of aerosols from the wildfires to Allentown, Pennsylvania, identified the densest regions of the smoke plumes, and provided a map of wildfire locations in southeastern Canada. By integrating these datasets, we traced how wildfire smoke transported aerosols from the source at the ground level.

      Michele Iraci
      Trends and Transport of Tropospheric Ozone From New York City to Connecticut in the Summer of 2023
      Michele Iraci
      Tropospheric Ozone, or O₃, is a criteria pollutant contributing to most of Connecticut and New York City’s poor air quality days. It has adverse effects on human health, particularly for high-risk individuals. Ozone is produced by nitrogen oxides and volatile organic compounds from fuel combustion reacting with sunlight. The Ozone Transport Region (OTR) is a collection of states in the Northeast and Mid-Atlantic United States that experience cross-state pollution of O₃. Connecticut has multiple days a year where O₃ values exceed the National Ambient Air Quality Standards requiring the implementation of additional monitoring and standards because it falls in the OTR. Partially due to upstream transport from New York City, Connecticut experiences increases in O₃ concentrations in the summer months. Connecticut has seen declines in poor air quality days from O₃ every year due to the regulations on ozone and its precursors. We use ground-based Lidar, Air Quality System data, and a back-trajectory model to examine a case of ozone enhancement in Connecticut caused by air pollutants from New York between June and August 2023. In this time period, Connecticut’s ozone enhancement was caused by air pollutants from New York City. As a result, New York City and Connecticut saw similar O₃ spikes and decline trends. High-temperature days increase O₃ in both places, and wind out of the southwest may transport O₃ to Connecticut. Production and transport of O₃ from New York City help contribute to Connecticut’s poor air quality days, resulting in the need for interstate agreements on pollution management.

      Stefan Sundin
      Correlations Between the Planetary Boundary Layer Height and the Lifting Condensation Level
      Stefan Sundin
      The Planetary Boundary Layer (PBL) characterizes the lowest layer in the atmosphere that is coupled with diurnal heating at the surface. The PBL grows during the day as solar heating causes pockets of air near the surface to rise and mix with cooler air above. Depending on the type of terrain and surface albedo that receives solar heating, the depth of the PBL can vary to a great extent. This makes PBL height (PBLH) a difficult variable to quantify spatially and temporally. While several methods have been used to obtain the PBLH such as wind profilers and lidar techniques, there is still a level of uncertainty associated with PBLH. One method of predicting seasonal PBLH fluctuation and potentially lessening uncertainty that will be discussed in this study is recognizing a correlation in PBLH with the lifting condensation level (LCL). Like the PBL, the LCL is used as a convective parameter when analyzing upper air data, and classifies the height in the atmosphere at which a parcel becomes saturated when lifted by a forcing mechanism, such as a frontal boundary, localized convergence, or orographic lifting. A reason to believe that PBLH and LCL are interconnected is their dependency on both the amount of surface heating and moisture that is present in the environment. These thermodynamic properties are of interest in heavily populated metropolitan areas within the Great Plains, as they are more susceptible to severe weather outbreaks and associated economic losses. Correlations between PBLH and LCL over the Minneapolis-St. Paul metropolitan statistical area during the summer months of 2019-2023 will be discussed.

      Angelica Kusen
      Coupling of Chlorophyll-a Concentrations and Aerosol Optical Depth in the Subantarctic Southern Ocean and South China Sea (2019-2021)
      Angelica Kusen
      Air-sea interactions form a complex feedback mechanism, whereby aerosols impact physical and biogeochemical processes in marine environments, which, in turn, alter aerosol properties. One key indicator of these interactions is chlorophyll-a (Chl-a), a pigment common to all phytoplankton and a widely used proxy for primary productivity in marine ecosystems. Phytoplankton require soluble nutrients and trace metals for growth, which typically come from oceanic processes such as upwelling. These nutrients can also be supplied via wet and dry deposition, where atmospheric aerosols are removed from the atmosphere and deposited into the ocean. To explore this interaction, we analyze the spatial and temporal variations of satellite-derived chl-a and AOD, their correlations, and their relationship with wind patterns in the Subantarctic Southern Ocean and the South China Sea from 2019 to 2021, two regions with contrasting environmental conditions.
      In the Subantarctic Southern Ocean, a positive correlation (r²= 0.26) between AOD and Chl-a was found, likely due to dust storms following Austrian wildfires. Winds deposit dust aerosols rich in nutrients, such as iron, to the iron-limited ocean, enhancing phytoplankton photosynthesis and increasing chl-a. In contrast, the South China Sea showed no notable correlation (r² = -0.02) between AOD and chl-a. Decreased emissions due to COVID-19 and stricter pollution controls likely reduced the total AOD load and shifted the composition of aerosols from anthropogenic to more natural sources.
      These findings highlight the complex interrelationship between oceanic biological activity and the chemical composition of the atmosphere, emphasizing that atmospheric delivery of essential nutrients, such as iron and phosphorus, promotes phytoplankton growth. Finally, NASA’s recently launched PACE mission will contribute observations of phytoplankton community composition at unprecedented scale, possibly enabling attribution of AOD levels to particular groups of phytoplankton.

      Chris Hautman
      Estimating CO₂ Emission from Rocket Plumes Using in Situ Data from Low Earth Atmosphere
      Chris Hautman
      Rocket emissions in the lower atmosphere are becoming an increasing environmental concern as space exploration and commercial satellite launches have increased exponentially in recent years. Rocket plumes are one of the few known sources of anthropogenic emissions directly into the upper atmosphere. Emissions in the lower atmosphere may also be of interest due to their impacts on human health and the environment, in particular, ground level pollutants transported over wildlife protected zones, such as the Everglades, or population centers near launch sites. While rockets are a known source of atmospheric pollution, the study of rocket exhaust is an ongoing task. Rocket exhaust can have a variety of compositions depending on the type of engine, the propellants used, including fuels, oxidizers, and monopropellants, the stoichiometry of the combustion itself also plays a role. In addition, there has been increasing research into compounds being vaporized in atmospheric reentry. These emissions, while relatively minimal compared to other methods of travel, pose an increasing threat to atmospheric stability and environmental health with the increase in human space activity. This study attempts to create a method for estimating the total amount of carbon dioxide released by the first stage of a rocket launch relative to the mass flow of RP-1, a highly refined kerosene (C₁₂H₂₆)), and liquid oxygen (LOX) propellants. Particularly, this study will focus on relating in situ CO₂ emission data from a Delta II rocket launch from Vandenberg Air Force Base on April 15, 1999, to CO₂ emissions from popular modern rockets, such as the Falcon 9 (SpaceX) and Soyuz variants (Russia). The findings indicate that the CO₂ density of any RP-1/LOX rocket is 6.9E-7 times the mass flow of the sum of all engines on the first stage. The total mass of CO₂ emitted can be further estimated by modeling the volume of the plume as cylindrical. Therefore, the total mass can be calculated as a function of mass flow and first stage main engine cutoff. Future CO₂ emissions on an annual basis are calculated based on these estimations and anticipated increases in launch frequency.


      Return to 2024 SARP Closeout Share
      Details
      Last Updated Nov 22, 2024 Related Terms
      General Explore More
      8 min read SARP East 2024 Ocean Remote Sensing Group
      Article 21 mins ago 10 min read SARP East 2024 Hydroecology Group
      Article 21 mins ago 11 min read SARP East 2024 Terrestrial Fluxes Group
      Article 22 mins ago View the full article
    • By NASA
      10 min read
      Preparations for Next Moonwalk Simulations Underway (and Underwater)
      Return to 2024 SARP Closeout Faculty Advisors:
      Dr. Dom Ciruzzi, College of William & Mary
      Graduate Mentor:
      Marley Majetic, Pennsylvania State University

      Marley Majetic, Graduate Mentor
      Marley Majetic, graduate mentor for the 2024 SARP Hydroecology group, provides an introduction for each of the group members and shares behind-the scenes moments from the internship.
      Jordan DiPrima
      How are different land cover types affected by land subsidence on the U.S. Atlantic Coast?
      Jordan DiPrima
      Land subsidence is a frequently overlooked geologic hazard that is caused by natural processes and, more recently, anthropogenic stressors. The goal of this study is to observe subsidence trends and hotspots among land cover types on Virginia’s Eastern Shore and Long Island, New York. This study utilizes interferometric synthetic aperture radar, or InSAR, satellite data from Sentinel-1 to map vertical land motion from 2017 to 2023. Land cover data were sourced from Landsat 8 satellite imagery. Subsidence was mapped within the following land cover types on the Eastern Shore: urban, wetland, cropland, temperate or sub-polar grassland, temperate or sub-polar shrubland, mixed forest, and temperate or subpolar needleleaf forest. These land cover types have mean vertical velocities ranging from -0.2 mm/yr to -5.2 mm/yr. Results suggest that land subsidence is most severe in cropland areas on the Eastern Shore, with a mean vertical velocity of -5.2 mm/yr. In contrast, wetlands display the most subsidence on Long Island with a mean vertical velocity of -2.1 mm/yr. Long Island lacked distinct trends among land cover types and instead showed evidence of subsidence hotspots. These hotspots exist in the following land cover types: temperate or sub-polar grassland, barren lands, wetland, cropland, and temperate or sub-polar broadleaf deciduous forest. Overall, Eastern Shore croplands and Long Island wetlands were determined to be the most susceptible land cover types. These findings highlight regions at risk of sea level rise, flooding, and coastal erosion as a result of subsidence. With further research, we can map subsiding landscapes on a global scale to improve resource allocation and mitigation techniques.

      Isabelle Peterson
      Total Thermokarst Lake Changes on the Seward Peninsula, Alaska: 2016 to 2024
      Isabelle Peterson
      Thermokarst landscapes have and will continue to change as the arctic landscape warms due to climate change. Permafrost underlies much of these arctic landscapes, and as it melts, thermokarst landscapes are left behind. The Seward Peninsula in Alaska has an abundance of these landscapes, and thermokarst lakes are present in the northernmost portion. Several lakes have come and gone, but with increasing climate instability and warming of the area, there is a possibility of more permafrost melting, creating more of these lakes. To capture these changes, Harmonized Landsat Sentinel-2 (HLS) imagery were used to create annual lake maps of the northern portion of the Seward Peninsula from 2016 to 2024. Much of the methodology was informed from Jones et al. (2011); however, their study used eCognition, while the present study used ArcGIS Pro. This caused some differences in results likely due to the differences in software, satellite imagery, and the proposed study area. Lake number changes were observed annually. From this annual change, several 10 to 40 ha lakes disappeared and reappeared within the study period, along with smaller lakes filling in where larger lakes once were. Thermokarst lake drainage is a process described by Jones and Arp (2015) which has devastating geomorphological impacts on the surrounding area, creating large drainage troughs which diminish surrounding permafrost in a quick time frame. To capture these events and overall changes, satellite imagery is essential. This is especially true in remote regions which are hard to reach by foot and require flight missions to be scheduled over the area for aerial photography. However, LVIS and other higher resolution aerial instruments would provide higher accuracy when identifying smaller lakes, as satellite imagery does not accurately capture lakes below 1 ha in the study area. This assertion is made due to conflicting results compared to Jones et al (2011). While the methodologies of this study have been executed manually, Qin, Zhang, and Lu (2023) have proposed the idea of using Sentinel-2 imagery to map thermokarst lakes through automatic methods. While automatization has not yet been perfected, the potential is there and can be used to analyze thermokarst areas effectively. With more satellite imagery, annual, monthly, and potentially daily changes can be captured in favorable months to monitor changing landscapes in arctic regions. Thermokarst lakes have been changing, and monitoring them can help in the process of understanding the changing climate in arctic areas, especially through the lens melting permafrost.

      Emmanelle Cuasay
      Finding Refuge in Climate Crisis: Analyzing the Differences between Refugia and Non-Refugia in the Northern Philippines Using Remote Sensing
      Emmanelle Cuasay
      Refugia are areas that are characterized by stable environmental conditions that can act as a refuge for species as Earth’s climate warms. In this study, fourteen Harmonized Landsat Sentinel-2 images from February 2014 – March 2024 of the northern Philippines region were used. The region of interest is the terrestrial biome by Lake Taal. Normalized Difference Vegetation Index (NDVI) maps were created from all fourteen images to determine the NDVI 25th highest quartiles of the long-term average NDVI images and of a dry and wet year NDVI image. These values were then used to create refugia and non-refugia maps using ArcGIS Pro. Land cover data from Sentinel-2 and a digital elevation model (DEM), using the Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER), were plotted in ArcGIS Pro to determine the slope and aspect of the area. Global Ecosystems Dynamics Investigation (GEDI) data were used to look at forest height of the study area, and the distribution of forest height, slope, aspect, and elevation were plotted to determine their probability densities in refugia and non-refugia areas. Results of this study show increased biomass in refugia areas. This suggests that conservation practices are crucial to aid in the preservation of biodiversity and biomass within these refugia areas.

      Jayce Crayne
      Site-Based Observations of a Saharan Dust Storm’s Impacts on Evapotranspiration in North-Central Florida
      Jayce Crayne
      Saharan dust storms serve an important role in the western Atlantic’s climate in their contribution to Earth’s radiation budget, modulating sea surface temperatures (SSTs), fertilizing ecosystems, and suppressing cloud and precipitation patterns (Yuan et al., 2020). However, Saharan dust storms are expected to become less frequent in this region as SSTs continue to rise (Yuan et al., 2020). Predicting the climate response to this change requires a keen understanding of how the presence of these storms affect evapotranspiration (ET) and its indicators. This study utilizes site-based observational data from an AmeriFlux tower near Gainesville, FL recorded during a large dust storm in late June 2020. The storm’s progression was documented using satellite imagery from Aqua and Terra and aerosol optical depth (AOD) measurements from an Aerosol Robotic Network (AERONET) station co-located with the AmeriFlux tower. Indicators of ET such as surface air temperature, vapor pressure deficit, photosynthetic photon flux density, and net radiation were analyzed. Findings were compared to modeled ET and latent energy flux reanalysis data provided by the Global Land Data Assimilation System (GLDAS). Both model simulations and on-site observations support that ET decreased during the days dust concentrations were heaviest and for a short time thereafter. Cloud cover data adopted from meteorological aerodrome reports (METARs) provided by an automated surface observing system (ASOS) located in Gainesville showed that clouds were not a major contributor in decreasing ET during the days of heaviest dust. The results of this study show a considerable decrease in ET as a result of dust aerosols. Further research is necessary to determine whether changes in ET due to Saharan dust storms are significant enough to alter climates in the western Atlantic and, if so, what the climate response will be if the frequency of storms decreases.

      Brandon Wilson
      Predicting 2025 and 2028 dNBR and dNDIV for Csarf Smith River Complex / Evaluating the Effects of 2019 California Wildfire Fund
      Brandon Wilson
      Biodiverse regions across California remain vulnerable to harmful wildfires year round. Quantifying and measuring these regions’ wildfire resilience is necessary for understanding where/how to allocate environmental resources. Several ecological wildfire studies have been conducted utilizing artificial intelligence and remote sensing to analyze and predict biodiversity damage across wildfire prone regions, including Northern Algeria and Arkansas, USA. The current case study aims to analyze biodiversity damage from the 2023 Csarf Smith River Complex Fire in Six Rivers National Forest, California and predict the difference in Normalized Burn Ratio (dNBR) and difference in Normalized Difference Vegetation Index (dNDVI) for 2025 and 2028 using remote-sensing-based random forest (RF) regression. Furthermore, to observe, holistically, a practical method California has implemented to address state-wide wildfire damage, the 2019 California Wildfire Fund (AB 1054 and AB 111) was evaluated using the synthetic control method (SCM). For this case study, remote sensing data from the United States Geological Survey (USGS) and NASA (Landsat 9 Satellite C2 L2, TerraClimate and the Land Data Assimilation System) were utilized for processing relevant spectral indexes for the RF. Data from NOAA, Energy Information Agency, International Monetary Fund and Bureau of Economic Analysis were utilized as synthetic control datasets to evaluate the effects of the 2019 California Wildfire Fund. Elevated topography in this study area is susceptible to high severity burn effects, while less elevated topography burns less. This result affected dNBR and dNDVI predictions as elevated areas seemingly did not have strong resilience to rampant burns. This demonstrates a direct correlation to potential lower transpiration rates for elevated areas, warranting further analysis. Results of low variance, post-treatment, between the treated unit and the synthetic control unit, poses concern for the positive effect of the 2019 Wildfire Fund.

      Carrie Hashimoto
      Describing changes in evapotranspiration following the 2020 Creek Fire in the southern Sierra Nevada
      Carrie Hashimoto
      Climatic warming and high tree density have caused larger and more severe wildfires to occur in western United States forests over time. Wildfires affect both the hydrology and ecology of forests via alterations to the water balance (e.g., evapotranspiration, streamflow, infiltration, and more) and could shift vegetation communities and subsequent ecosystem structure and function. This project explores ecological characteristics of a landscape that predict the extent to which the Creek Fire in the southern Sierra Nevada has affected evapotranspiration. Strides in understanding of consequential evapotranspiration changes can create pathways to address emerging forest health challenges posed by similar western fires. For analysis, various remote sensing and modeled data were collected from OpenET, the North American Land Data Assimilation System, TerraClimate, Harmonized LandSat Sentinel-2 data, and the Shuttle Radar Topography Mission. Multiple linear regression and generalized additive models were constructed. Relative change in evapotranspiration served as the response variable. Model covariates included average temperature, total precipitation in the preceding months, average soil moisture, elevation, slope, aspect, northness, latitude, pre-fire normalized difference vegetation index (NDVI), and post-fire change in normalized burn ratio (dNBR). Best subset selection with cross validation demonstrated minimization of cross-validation error with a 7-covariate model. This reduced model yields lower complexity and more interpretability while sustaining an adjusted R2 of 0.626, compared to the full model’s adjusted R2 of 0.663. A reduced generalized additive model (GAM) with interaction terms drawn from the linear model variable selection demonstrated an adjusted R2 of 0.695, indicating a better fit that comes at the cost of reduced interpretability and higher computational requirements than the linear models. The goal of this work is to disentangle environmental indicators of post-fire evapotranspiration change, such that predictive modeling of future wildfire impacts on evapotranspiration can be achieved.


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      Last Updated Nov 22, 2024 Related Terms
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      8 min read SARP East 2024 Ocean Remote Sensing Group
      Article 21 mins ago 10 min read SARP East 2024 Atmospheric Science Group
      Article 21 mins ago 11 min read SARP East 2024 Terrestrial Fluxes Group
      Article 22 mins ago View the full article
    • By NASA
      11 min read
      Preparations for Next Moonwalk Simulations Underway (and Underwater)
      Return to 2024 SARP Closeout Faculty Advisors:
      Dr. Lisa Haber, Virginia Commonwealth University
      Dr. Brandon Alveshere, Virginia Commonwealth University
      Dr. Chris Gough, Virginia Commonwealth University
      Graduate Mentor:
      Mindy Priddy, Virginia Commonwealth University

      Mindy Priddy, Graduate Mentor
      Mindy Priddy, graduate mentor for the 2024 SARP Terrestrial Fluxes group, provides an introduction for each of the group members and shares behind-the scenes moments from the internship.

      Angelina De La Torre
      Using NDVI as a Proxy for GPP to Predict Carbon Dioxide Fluxes
      Angelina De La Torre
      Climate change, driven primarily by greenhouse gases, poses a threat to the future of our planet. Among these gases is carbon dioxide (CO₂), which has a much longer atmospheric residence time compared to other greenhouse gases. One potential factor in reducing atmospheric CO₂ enrichment is plant productivity. Gross Primary Productivity (GPP) estimates the amount of CO₂ fixed during photosynthesis. The Normalized Difference Vegetation Index (NDVI) provides insight into the health of an ecosystem by measuring the density and greenness of vegetation. Therefore, it can be inferred that there is a relationship between NDVI and GPP, as greener plants are likely more productive. In this study, we used NDVI as a proxy for GPP and analyzed the effect NDVI had on CO₂ fluxes during California’s wet season between January and March 2023 in a restored tidal freshwater wetland. GPP and CO₂ flux data were obtained from the Dutch Slough AmeriFlux tower in Oakley, California. Landsat data were used to calculate the average NDVI. The influence of NDVI on GPP was assessed using linear regression. A second linear regression was then performed using NDVI and CO₂ flux, of which GPP is one component. We anticipate that wetlands with greater vegetation density will have lower CO₂ emissions.

      Because Landsat data scans in 16-day intervals, daily variation in NDVI could not be observed. This translates to a frequency discrepancy between the Landsat and AmeriFlux data, as AmeriFlux towers measure in half-hour intervals. Additionally, the wet season represented was limited by data availability, as the data before 2023 were unavailable. Despite data limitations in this study, the outlined process could be repeated in various wetland and climate classifications for further analysis of a larger sample size. This study could assist in developing strategies to increase CO₂ sequestration in an attempt to slow the effects of climate change.

      Samarth Jayadev
      Using Machine Learning to Assess Relationships between NDVI and Net Carbon Exchange During the COVID-19 Pandemic
      Samarth Jayadev
      Understanding the movement of carbon between Earth’s land surface and atmosphere is essential for ecosystem monitoring, creating climate change mitigation strategies, and assessing the carbon budget on national to global scales. Measures of greenness serve as indicators of processes such as photosynthesis that control carbon exchange and are vital in modeling of carbon fluxes. NASA’s Orbiting Carbon Observatory (OCO-2) provides high quality measurements of column-averaged CO₂ concentrations that can be used to derive net carbon exchange (NCE), a measure of CO₂ flux between terrestrial ecosystems and the atmosphere.
      From OCO-2, NCE data collected at the land nadir, land glint satellite position combined with in situ sampling can provide accurate measurements on a 1°x1° scale suitable for carbon flux characterization across the contiguous United States (CONUS). Normalized difference vegetation index (NDVI), which ranges from -1 to +1, measures the greenness of vegetation, serving as an indicator of plant density and health. This can help to understand ecosystem to carbon-cycle interactions and be leveraged for determining patterns with NCE. We examined the relationship between NDVI and NCE across CONUS during 2020 using Gradient Boosting Decision Trees (GBDT) which specialize in classifying and predicting non-linear relationships. This algorithm takes multiple weak learners (decision trees) and combines their predictions in an iterative ensemble method to improve prediction accuracy. Feature and permutation importance tests found that January and August (trough and peak NDVI, respectively) were the highest weighted predictor variables related to NCE. The dataset was split in a 90% training 10% test ratio across latitude/longitude grid cells to assess and verify model performance. Using the mean squared error loss function and hyperparameters with optimal estimators, tree depth, sample split, and learning rate the algorithm was able to converge the test predictions to match the deviance of the training data. The gradient boosting model can be applied to different months and years of NDVI/NCE to further explore these relationships or a multitude of research questions. Further studies should consider integrating land use and land cover change variables such as bare land and urbanization to improve predictions of NCE.

      Makai Ogoshi
      Deep-learning Derived Spaceborne Canopy Structural Metrics Predict Forest Carbon Fluxes
      Makai Ogoshi
      Terrestrial and airborne lidar data products describing canopy structure are potent predictors of forest carbon fluxes, but whether satellite data products produce similarly robust indicators of canopy structure is not known. The assessment of contemporary spaceborne lidar and other remote sensing data products as predictors of carbon fluxes is crucial to next generation instrument and data product design and large-spatial scale modeling. We investigated relationships between deciduous broadleaf forest canopy structure, derived from deep-learning models created with lidar data from GEDI and optical imagery from Sentinel-2, and forest carbon exchange. These included comparisons to in-situ continuous net ecosystem exchange (NEE), gross primary production (GPP), and net primary production (NPP). We find that the mean  canopy height from the gridded spaceborne product has a strong correlation with forest NPP, similar to prior analysis with ground-based lidar (portable canopy lidar; PCL). For comparison to NPP, heights taken from the gridded spaceborne product were compared by overlapping the product with nine terrestrial forest sites from the National Ecological Observatory Network (NEON). We used standard deviation of canopy height as a measure of canopy structural complexity. Complexity derived from the gridded spaceborne product does not show the same strong correlation with NPP as found when using PCL. Mean annual GPP and NEE across five years were compared to the gridded spaceborne product at six Fluxnet2015-tower sites with continuous, gap-filled carbon flux data. When compared to in-situ flux tower data, neither mean canopy height nor structural complexity strongly correlate to annual NEE or GPP. Primarily, the finding that derived spaceborne products exhibit a strong correlation between forest canopy height and NPP will advance global-scale application of forest-carbon flux predictions. Secondarily, a variety of limitations highlight shortcomings in the current terrestrial flux data network. A small number of available study sites, both spatially and temporally, and lack of resolution in vertical complexity of canopy structure both contribute to uncertainty in assessing the relationships to NEE and GPP.

      Sebastian Reed
      Porewater Methane Concentrations Vary Significantly Across A Freshwater Tidal Wetland
      Sebastian Reed
      Methane is a potent greenhouse gas that is over 80 times more powerful than CO₂ at trapping heat and accounts for an estimated 30% of global temperature rise associated with climate change. The largest natural source of methane worldwide is wetlands. Despite the role of methane in driving climate change, the magnitude of global annual wetland methane flux remains highly uncertain. This study analyzes the effects of greenness (assessed using Normalized Difference Vegetation Index; NDVI), plant species composition, rooting depth, atmospheric methane concentration, and plant longevity on porewater methane concentration at the Kimages Rice Rivers Center tidal freshwater wetland. Samples for atmospheric and porewater concentrations were conducted in situ in June 2024. For each sampling location (n = 23) we collected whole air samples (WAS) 2m above the marsh surface and porewater samples 5cm below the marsh surface. We visually assessed species composition at each sample location, with 12 species of wetland plants present overall. We used the TRY plant database to find the rooting depth, leaf nitrogen content, and lifespan of each species. Drone multispectral data from 2023 was used to estimate NDVI values. These variables were compared to the pore water methane concentration via stepwise linear regression. Leaf N content, NDVI, plant species, and WAS sampling did not show statistically significant correlation to porewater methane concentration. Rooting depth showed a slight positive correlation with porewater methane (alpha = 0.1, p = 0.08, R^2 = 0.1). Samples with only perennial plants (as opposed to annual plants) had a higher mean value of porewater methane (p = 0.1). Analyzing porewater methane provides insight as to what wetland components affect methanogenesis and methane release, which aids in assessing which plant functional traits are most responsible for driving or mitigating climate change. Results from this study and future research in this area has the potential to more accurately assess how methane cycles through wetlands to the atmosphere.

      Nohemi Rodarte
      Understanding the vertical profile of CO₂ concentration: How carbon dioxide levels change with altitude
      Nohemi Rodarte
      Carbon dioxide (CO₂) is one of the main greenhouse gasses that contribute to global warming.While the relationship between CO₂ concentrations and land cover types, such as forests and urban areas, is well documented, there is limited knowledge of how CO₂ concentrations vary with altitude at fine spatial scales. Guided by our hypothesis that CO₂ levels vary with altitude and increase with elevation, we used airborne data collected from the B200 aircraft, which flew at different altitudes (400 to 1200 feet) above the urban area of Hopewell, Virginia, between 9:40 AM and 10:40 AM. We analyzed the CO₂ concentrations recorded by the flight to obtain the median and range for each 100 feet of altitude. Our results reveal that carbon dioxide concentrations varied significantly across the range of altitudes investigated. Within the area studied, CO₂ concentrations were found to range between 410 and 470 ppm. The distribution of these concentrations along the altitude gradient shows a bimodal pattern, with notable peaks at altitudes of 700 to 800 feet and 1100 to 1200 feet. Although CO₂ levels were present at all measured altitudes, there was a noticeable drop in the mean concentration at 800 feet,which then stabilized until reaching 1,000 feet before rising again. This pattern indicates that the concentrations of this greenhouse gas are not uniformly distributed with altitude, but rather vary significantly, showing higher concentrations at certain elevations and lower concentrations at others. The CO₂ distribution fluctuates with altitude, showing higher or lower levels at specific heights rather than a smooth gradient, indicating that altitude impacts CO₂ concentrations. While we did not identify the drivers of this change, future studies could evaluate how factors such as surface emissions, atmospheric mixing, and local conditions may contribute to vertical CO₂ profiles, since the altitudes we considered in this research are within the troposphere.

      Camille Shaw
      Linking NDVI with CO₂ and CH₄ Fluxes: Insights into Vegetation and Urban Source-Sink Dynamics in the Great Dismal Swamp
      Camille Shaw
      In recent years, carbon dioxide, methane, and other greenhouse gases have gained attention because of their contribution to the rise in Earth’s global mean temperature. Methane and carbon dioxide have various sources and sinks, but an expanding array of sources have created a need to assess ongoing change in carbon balance. This study aims to quantify the relationship between Normalized Difference Vegetation Index, or NDVI, and methane and carbon dioxide fluxes. We measured carbon dioxide and methane concentrations within the boundary layer using the PICARRO instrument, focusing on the Great Dismal Swamp, a forested wetland, and surrounding areas in the Eastern Mid-Atlantic Region. Data collection occurred at various times of day and along different flight paths in 2016, 2017, and 2024, with each year representing data from a single season, either spring or fall, for temporal analysis. We calculated methane and carbon dioxide fluxes along the flight paths using airborne eddy covariance, a method for capturing accurate flux measurements while accounting for the mixing of gases in the boundary layer caused by heat. Additionally, we calculated NDVI for this area using NASA’s Landsat 8 and 9 satellite imagery. Analysis of the afternoon flight data revealed a negative linear correlation between NDVI and carbon dioxide flux. Urban areas, characterized by low NDVI, exhibit a positive carbon dioxide flux as a consequence of emissions from vehicles, while forested areas, with high NDVI, show a negative carbon dioxide flux because of photosynthesis. In contrast, methane flux shows minimal correlation with NDVI. The lack of correlation arises because forested wetlands, with high NDVI, emit substantial amounts of methane, while urban areas, despite having low NDVI, still produce significant methane emissions from landfills and industrial activities. Future research could further investigate how seasonal and diurnal variations influence the correlations between NDVI and greenhouse gases by collecting comprehensive data across all seasons within a given year and at various times of the day.

      Return to 2024 SARP Closeout Share
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      Last Updated Nov 22, 2024 Related Terms
      General Explore More
      8 min read SARP East 2024 Ocean Remote Sensing Group
      Article 21 mins ago 10 min read SARP East 2024 Atmospheric Science Group
      Article 21 mins ago 10 min read SARP East 2024 Hydroecology Group
      Article 21 mins ago View the full article
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