пятница, 3 августа 2018 г.

Segontium Roman Fort, Caernarfon, North Wales, 1.8.18.The scale…

Segontium Roman Fort, Caernarfon, North Wales, 1.8.18.

The scale of Segontium meant that at its height it must have been visible from many locations on both sides of the Menai Straits. Built on a raised plateau, the fort made a physical assertion against the freedoms of the local populace.

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Planetary Defense Has New Tool in Weather Satellite Lightning Detector

Asteroid Watch logo.

August 2, 2018

NASA’s efforts to better understand asteroid impacts has found unexpected support from a new satellite sensor designed to detect lightning. New research published in the journal Meteoritics and Planetary Science finds that the new Geostationary Lightning Mapper, or GLM, on two weather satellites is able to pick up signals of meteors in Earth’s atmosphere.

“GLM detects these meteors when they become brighter than the full Moon,” says lead author and meteor astronomer Peter Jenniskens of the SETI Institute and NASA’s Ames Research Center in California’s Silicon Valley. “Meteors that bright are called ‘bolides’ and they are caused mainly by the impact of small asteroids.”

Image above: On December 29, 2017, the Geostationary Lightning Mapper, an instrument flying on board two weather satellites, detected a bright meteor in Earth’s atmosphere over the western Atlantic Ocean. Image Credits: NASA/Lockheed Martin.

Jenniskens’ work on meteors contributes to the NASA Ames Asteroid Threat Assessment Program, which helps improve information for impact prediction warnings by studying how asteroids fragment as they travel through the atmosphere.

“The range of altitudes over which asteroids deposit their kinetic energy — the energy of their motion — determines how dangerous the shock waves are that can cause damage on the ground,” says Eric Stern, a research scientist at Ames who is the entry modeling lead for the program. “The light profiles derived from GLM data are slated now to be used in a future version of NASA’s automated bolide reporting system.”

The Geostationary Lightning Mapper, built by Lockheed Martin, was designed for mapping lightning flashes over vast geographic regions. The instrument captures 500 images per second of Earth from geostationary orbit, in which the satellite is always in the same position with respect to the rotating Earth, more than 22,000 miles up.

Image above: The bright flash produced by the December 2017 meteor was picked up by the Geostationary Lightning Mapper. This image shows one moment of that meteor event, which released three kilotons of energy into the atmosphere. In the image inset, red represents the bright meteor, while blue indicates the faint light reflected off the ocean surface and the signal caused by the instrument recovering from the bright exposure. Image Credits: NASA/Lockheed Martin.

“The instrument views Earth in only a narrow range of wavelengths of light,” said Samantha Edgington, GLM chief scientist at Lockheed Martin, who led the effort to develop the processing pipeline that now provides lightning data to weather forecasters. “Since most of the light is blocked, we were surprised to see how readily the instrument detected the meteors.”

GLM is one of several instruments onboard the new Geostationary Operational Environmental Satellites-16 and -17, which are operated by the National Atmospheric and Oceanic Administration.

“Although most lightning flashes are very brief, the relatively long-duration signals of bolides are not filtered out of the data,” said NOAA physical scientist Scott Rudlosky. “That’s because GLM also was designed to measure a longer-lasting lightning type that is known to play a key role in lightning-ignited wild fires.”

The ten bolides discussed in the paper were observed with the first GLM instrument on board GOES-16, which was launched in November 2016.

Animation above: Slow-motion movie of the December 2017 meteor impacting Earth’s atmosphere. Individual pixels in the Geostationary Lightning Mapper’s sensor are illuminated in successive frames. Animation Credits: NASA/Lockheed Martin.

“The first bolide we found in GLM data was on Feb. 6, 2017; more than 500 people reported seeing this event over Wisconsin that day,” said Jenniskens. “Meteorites likely fell in Lake Michigan but were never recovered.”

Other detected bolides show different manners of fragmentation. They include one that caused a meteorite fall in Canada and another large, explosive event over the western Atlantic Ocean of a rare size that occurs only once a year.

The Asteroid Threat Assessment Program is funded by the NASA Planetary Defense Coordination Office. The scientific paper is available online in the journal Meteoritics and Planetary Science: http://dx.doi.org/10.1111/maps.13137

Related links:

Asteroids: https://www.nasa.gov/mission_pages/asteroids/main/index.html

Meteors & Meteorites: http://www.nasa.gov/topics/solarsystem/features/watchtheskies/index.html

More information about asteroids and near-Earth objects is at these sites:



Images (mentioned), Animation (mentioned), Text, Credits: NASA/Abigail Tabor.

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Hubble Images Milky Way’s Big Sister

NASA – Hubble Space Telescope patch.

August 2, 2018

This image taken by the NASA/ESA Hubble Space Telescope’s Wide Field Camera 3 (WFC3) shows a beautiful spiral galaxy called NGC 6744. At first glance, it resembles our Milky Way albeit larger, measuring more than 200,000 light-years across compared to a 100,000-light-year diameter for our home galaxy.

NGC 6744 is similar to our home galaxy in more ways than one. Like the Milky Way, NGC 6744 has a prominent central region packed with old yellow stars. Moving away from the galactic core, one can see parts of the dusty spiral arms painted in shades of pink and blue; while the blue sites are full of young star clusters, the pink ones are regions of active star formation, indicating that the galaxy is still very lively.

In 2005, a supernova named 2005at (not visible in this image) was discovered within NGC 6744, adding to the argument of this galaxy’s liveliness. SN 2005at is a Type Ic supernova, formed when a massive star collapses on itself and loses its hydrogen envelope.

Hubble Space Telescope (HST)

For more information about Hubble, visit:


Image, Animation,  Credits: ESA/Hubble & NASA; acknowledgment: Judy Schmidt/Text Credits: ESA (European Space Agency)/NASA/Rob Garner.

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HiPOD (3 August 2018): Light-Toned Layered Deposits along…

HiPOD (3 August 2018): Light-Toned Layered Deposits along Northeast Melas Chasma Wallrock 

   – With this image, we’re looking for layering and fracture patterns to understand deposition process. (300 km above the surface. Black and white is less than 5 km across; enhanced color is less than 1 km.) 

NASA/JPL/University of Arizona


Hendre Waelod (Allor Molloch) Prehistoric Burial Chamber, nr…

Hendre Waelod (Allor Molloch) Prehistoric Burial Chamber, nr Conwy, North Wales, 1.8.18.

This is only the second time I have visited this site and in Summer the stones seem even more substantial in bright light.

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NASA Mars Exploration Rover Status Report

NASA – Mars Exploration Rover B (MER-B) patch.

August 2, 2018

t’s the beginning of the end for the planet-encircling dust storm on Mars. But it could still be weeks, or even months, before skies are clear enough for NASA’s Opportunity rover to recharge its batteries and phone home. The last signal received from the rover was on June 10.

Scientists observing the global event — which is actually caused by a series of local and regional storms throwing dust into the Martian atmosphere — say that, as of Monday, July 23, more dust is falling out than is being raised into the planet’s thin air. That means the event has reached its decay phase, when dust-raising occurs in ever smaller areas, while others stop raising dust altogether.

Graphic above: This graphic compares atmospheric opacity in different Mars years from the point of view of NASA’s Opportunity rover. The green spike in 2018 (Mars Year 34) shows how quickly the global dust storm building at Mars blotted out the sky. A previous dust storm in 2007 (red, Mars Year 28) was slower to build. The vertical axis shows atmospheric opacity and the horizontal axis shows the Martian season, which is measured by where the Sun is in the Martian sky compared to its apparent position on Mars’ northern spring equinox. Graphic Credits: NASA/JPL-Caltech/TAMU.

Surface features in many areas are beginning to re-appear as seen from orbit. This should even be apparent through telescopes on the ground: Next week, Mars will make its closest approach to Earth since 2003 — a particularly good time for observing the Red Planet.  Meanwhile, in Gale Crater, the nuclear-powered Mars Science Laboratory/Curiosity rover has noted a decline in dust overhead.

Temperatures in the middle atmosphere of Mars are no longer rising, and in some areas are starting to decrease. That indicates less solar heating by the dust.

Mars Exploration Rover. Image Credits: NASA/JPL-Calttech

The changes were spotted by the Mars Color Imager (MARCI), a wide-angle camera, and by the Mars Climate Sounder (MCS), a temperature profiler, on NASA’s Mars Reconnaissance Orbiter (MRO). MARCI is managed by Malin Space Science Systems in San Diego. MSL, MRO and MCS are managed by NASA’s Jet Propulsion Laboratory.

All of NASA’s Mars spacecraft have been observing the storm, both to support the Opportunity mission and to collect unique science about this global phenomenon.

Related articles:

Martian Dust Storm Grows Global: Curiosity Captures Photos of Thickening Haze

NASA Encounters the Perfect Storm for Science

Shades of Martian Darkness

Related link:

Mars Exploration Rovers (Spirit and Opportunity): https://www.nasa.gov/mission_pages/mer/index.html

Image, Graphic (mentioned), Text, Credits: NASA/Tony Greicius/JPL/Andrew Good.

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Artistic Portrait of Jupiter

NASA – JUNO Mission logo.

August 3 2018

Tumultuous tempests in Jupiter’s northern hemisphere are seen in this portrait taken by NASA’s Juno spacecraft.

Like our home planet, Jupiter has cyclones and anticyclones, along with fast-moving jet streams that circle its globe. This image captures a jet stream, called Jet N6, located on the far right of the image. It is next to an anticyclonic white oval that is the brighter circular feature in the top right corner. The North North Little Red Spot is also visible in this view.

The image was taken at 10 p.m. PDT on July 15, 2018 (1 a.m. EDT on July 16), as the spacecraft performed its 14th close flyby of Jupiter. At the time, Juno was about 10,600 miles (17,000 kilometers) from the planet’s cloud tops, above a latitude of 59 degrees.

Citizen scientists Brian Swift and Seán Doran created this image using data from the spacecraft’s JunoCam imager. The image has been rotated clockwise so that north is to the right. The stars were artfully added to the background for effect.

JunoCam’s raw images are available at http://www.missionjuno.swri.edu/junocam for the public to peruse and process into image products.

More information about Juno is online at http://www.nasa.gov/juno and http://missionjuno.swri.edu.

Juno orbiting Jupiter

NASA’s Jet Propulsion Laboratory manages the Juno mission for the principal investigator, Scott Bolton, of Southwest Research Institute in San Antonio. Juno is part of NASA’s New Frontiers Program, which is managed at NASA’s Marshall Space Flight Center in Huntsville, Alabama, for NASA’s Science Mission Directorate. Lockheed Martin Space Systems, Denver, built the spacecraft. Caltech in Pasadena, California, manages JPL for NASA.

Image, Animation, Text, Credits: NASA/JPL-Caltech/SwRI/MSSS/Brian Swift and Sean Doran.

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The four outer gates of Hardknott Roman Fort, Cumbria,…

The four outer gates of Hardknott Roman Fort, Cumbria, 31.7.18.

Like all typical Roman forts, the outer perimeter had four main gates in the centre of each of the walls. These exited to the Roman road and the nearby parade grounds.

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Astronomers Uncover New Clues to the Star that Wouldn’t Die

Credits: NASA, ESA, and A. Feild (STScI)

Credits: NASA, ESA, and G. Bacon (STScI)

What happens when a star behaves like it exploded, but it’s still there?

About 170 years ago, astronomers witnessed a major outburst by Eta Carinae, one of the brightest known stars in the Milky Way galaxy. The blast unleashed almost as much energy as a standard supernova explosion.

Yet Eta Carinae survived.

An explanation for the eruption has eluded astrophysicists. They can’t take a time machine back to the mid-1800s to observe the outburst with modern technology.

However, astronomers can use nature’s own “time machine,” courtesy of the fact that light travels at a finite speed through space. Rather than heading straight toward Earth, some of the light from the outburst rebounded or “echoed” off of interstellar dust, and is just now arriving at Earth. This effect is called a light echo. The light is behaving like a postcard that got lost in the mail and is only arriving 170 years later.

By performing modern astronomical forensics of the delayed light with ground-based telescopes, astronomers uncovered a surprise. The new measurements of the 1840s eruption reveal material expanding with record-breaking speeds up to 20 times faster than astronomers expected. The observed velocities are more like the fastest material ejected by the blast wave in a supernova explosion, rather than the relatively slow and gentle winds expected from massive stars before they die.

Based on this data, researchers suggest that the eruption may have been triggered by a prolonged stellar brawl among three rowdy sibling stars, which destroyed one star and left the other two in a binary system. This tussle may have culminated with a violent explosion when Eta Carinae devoured one of its two companions, rocketing more than 10 times the mass of our Sun into space. The ejected mass created gigantic bipolar lobes resembling the dumbbell shape seen in present-day images.

The results are reported in a pair of papers by a team led by Nathan Smith of the University of Arizona in Tucson, Arizona, and Armin Rest of the Space Telescope Science Institute in Baltimore, Maryland.

The light echoes were detected in visible-light images obtained since 2003 with moderate-sized telescopes at the Cerro Tololo Inter-American Observatory in Chile. Using larger Magellan telescopes at the Carnegie Institution for Science’s Las Campanas Observatory and the Gemini South Observatory, both also located in Chile, the team then used spectroscopy to dissect the light, allowing them to measure theejecta’s expansion speeds. They clocked material zipping along at more than 20 million miles per hour (fast enough to travel from Earth to Pluto in a few days).

The observations offer new clues to the mystery surrounding the titanic convulsion that, at the time, made Eta Carinae the second-brightest nighttime star seen in the sky from Earth between 1837 and 1858. The data hint at how it may have come to be the most luminous and massive star in the Milky Way galaxy.

“We see these really high velocities in a star that seems to have had a powerful explosion, but somehow the star survived,” Smith explained. “The easiest way to do this is with a shock wave that exits the star and accelerates material to very high speeds.”

Massive stars normally meet their final demise in shock-driven events when their cores collapse to make a neutron star or black hole. Astronomers see this phenomenon in supernova explosions where the star is obliterated. So how do you have a star explode with a shock-driven event, but it isn’t enough to completely blow itself apart? Some violent event must have dumped just the right amount of energy onto the star, causing it to eject its outer layers. But the energy wasn’t enough to completely annihilate the star.

One possibility for just such an event is a merger between two stars, but it has been hard to find a scenario that could work and match all the data on Eta Carinae.

The researchers suggest that the most straightforward way to explain a wide range of observed facts surrounding the eruption is with an interaction of three stars, where the objects exchange mass.

If that’s the case, then the present-day remnant binary system must have started out as a triple system. “The reason why we suggest that members of a crazy triple system interact with each other is because this is the best explanation for how the present-day companion quickly lost its outer layers before its more massive sibling,” Smith said.

In the team’s proposed scenario, two hefty stars are orbiting closely and a third companion is orbiting farther away. When the most massive of the close binary stars nears the end of its life, it begins to expand and dumps most of its material onto its slightly smaller sibling.

The sibling has now bulked up to about 100 times the mass of our Sun and is extremely bright. The donor star, now only about 30 solar masses, has been stripped of its hydrogen layers, exposing its hot helium core.

Hot helium core stars are known to represent an advanced stage of evolution in the lives of massive stars. “From stellar evolution, there’s a pretty firm understanding that more massive stars live their lives more quickly and less massive stars have longer lifetimes,” Rest explained. “So the hot companion star seems to be further along in its evolution, even though it is now a much less massive star than the one it is orbiting. That doesn’t make sense without a transfer of mass.”

The mass transfer alters the gravitational balance of the system, and the helium-core star moves farther away from its monster sibling. The star travels so far away that it gravitationally interacts with the outermost third star, kicking it inward. After making a few close passes, the star merges with its heavyweight partner, producing an outflow of material.

In the merger’s initial stages, the ejecta is dense and expanding relatively slowly as the two stars spiral closer and closer. Later, an explosive event occurs when the two inner stars finally join together, blasting off material moving 100 times faster. This material eventually catches up with the slow ejecta and rams into it like a snowplow, heating the material and making it glow. This glowing material is the light source of the main historical eruption seen by astronomers a century and a half ago.

Meanwhile, the smaller helium-core star settles into an elliptical orbit, passing through the giant star’s outer layers every 5.5 years. This interaction generates X-ray emitting shock waves.

A better understanding of the physics of Eta Carinae’s eruption may help to shed light on the complicated interactions of binary and multiple stars, which are critical for understanding the evolution and death of massive stars.

The Eta Carinae system resides 7,500 light-years away inside the Carina nebula, a vast star-forming region seen in the southern sky.

The team published its findings in two papers, which appear online Aug. 2 in The Monthly Notices of the Royal Astronomical Society.

The Hubble Space Telescope is a project of international cooperation between NASA and ESA (European Space Agency). NASA’s Goddard Space Flight Center in Greenbelt, Maryland, manages the telescope. The Space Telescope Science Institute (STScI) in Baltimore, Maryland, conducts Hubble science operations. STScI is operated for NASA by the Association of Universities for Research in Astronomy in Washington, D.C.


Illustration: NASA, ESA, and A. Feild (STScI)
Science: NSF and AURA

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Donna Weaver / Ray Villard
Space Telescope Science Institute, Baltimore, Maryland
410-338-4493 / 410-338-4514

dweaver@stsci.edu / villard@stsci.edu

Nathan Smith
University of Arizona, Tucson


Armin Rest
Space Telescope Science Institute, Baltimore, Maryland


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VLA Detects Possible Extrasolar Planetary-Mass Magnetic Powerhouse

Artist’s conception of SIMP J01365663+0933473, an object with 12.7 times the mass of Jupiter, but a magnetic field 200 times more powerful than Jupiter’s. This object is 20 light-years from Earth. Credit: Chuck Carter, NRAO/AUI/NSF.  Hi-res image

Object is at boundary between giant planet and brown dwarf

Astronomers using the National Science Foundation’s Karl G. Jansky Very Large Array (VLA) have made the first radio-telescope detection of a planetary-mass object beyond our Solar System. The object, about a dozen times more massive than Jupiter, is a surprisingly strong magnetic powerhouse and a “rogue,” traveling through space unaccompanied by any parent star.

“This object is right at the boundary between a planet and a brown dwarf, or ‘failed star,’ and is giving us some surprises that can potentially help us understand magnetic processes on both stars and planets,” said Melodie Kao, who led this study while a graduate student at Caltech, and is now a Hubble Postdoctoral Fellow at Arizona State University.

Brown dwarfs are objects too massive to be considered planets, yet not massive enough to sustain nuclear fusion of hydrogen in their cores — the process that powers stars. Theorists suggested in the 1960s that such objects would exist, but the first one was not discovered until 1995. They originally were thought to not emit radio waves, but in 2001 a VLA discovery of radio flaring in one revealed strong magnetic activity.

Subsequent observations showed that some brown dwarfs have strong auroras, similar to those seen in our own Solar System’s giant planets. The auroras seen on Earth are caused by our planet’s magnetic field interacting with the solar wind. However, solitary brown dwarfs do not have a solar wind from a nearby star to interact with. How the auroras are caused in brown dwarfs is unclear, but the scientists think one possibility is an orbiting planet or moon interacting with the brown dwarf’s magnetic field, such as what happens between Jupiter and its moon Io.

The strange object in the latest study, called SIMP J01365663+0933473, has a magnetic field more than 200 times stronger than Jupiter’s. The object was originally detected in 2016 as one of five brown dwarfs the scientists studied with the VLA to gain new knowledge about magnetic fields and the mechanisms by which some of the coolest such objects can produce strong radio emission. Brown dwarf masses are notoriously difficult to measure, and at the time, the object was thought to be an old and much more massive brown dwarf.

Last year, an independent team of scientists discovered that SIMP J01365663+0933473 was part of a very young group of stars. Its young age meant that it was in fact so much less massive that it could be a free-floating planet — only 12.7 times more massive than Jupiter, with a radius 1.22 times that of Jupiter. At 200 million years old and 20 light-years from Earth, the object has a surface temperature of about 825 degrees Celsius, or more than 1500 degrees Fahrenheit. By comparison, the Sun’s surface temperature is about 5,500 degrees Celsius.

The difference between a gas giant planet and a brown dwarf remains hotly debated among astronomers, but one rule of thumb that astronomers use is the mass below which deuterium fusion ceases, known as the “deuterium-burning limit”, around 13 Jupiter masses.

Simultaneously, the Caltech team that originally detected its radio emission in 2016 had observed it again in a new study at even higher radio frequencies and confirmed that its magnetic field was even stronger than first measured.

“When it was announced that SIMP J01365663+0933473 had a mass near the deuterium-burning limit, I had just finished analyzing its newest VLA data,” said Kao.

The VLA observations provided both the first radio detection and the first measurement of the magnetic field of a possible planetary mass object beyond our Solar System.

Such a strong magnetic field “presents huge challenges to our understanding of the dynamo mechanism that produces the magnetic fields in brown dwarfs and exoplanets and helps drive the auroras we see,” said Gregg Hallinan, of Caltech.

“This particular object is exciting because studying its magnetic dynamo mechanisms can give us new insights on how the same type of mechanisms can operate in extrasolar planets — planets beyond our Solar System. We think these mechanisms can work not only in brown dwarfs, but also in both gas giant and terrestrial planets,” Kao said.

“Detecting SIMP J01365663+0933473 with the VLA through its auroral radio emission also means that we may have a new way of detecting exoplanets, including the elusive rogue ones not orbiting a parent star,” Hallinan said.

Kao and Hallinan worked with J. Sebastian Pineda who also was a graduate student at Caltech and is now at the University of Colorado Boulder, David Stevenson of Caltech, and Adam Burgasser of the University of California San Diego. They are reporting their findings in the Astrophysical Journal.

The National Radio Astronomy Observatory is a facility of the National Science Foundation, operated under cooperative agreement by Associated Universities, Inc.


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Dave Finley, Public Information Officer
(575) 835-7302

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2018 August 3 Central Lunar Eclipse Image Credit &…

2018 August 3

Central Lunar Eclipse
Image Credit & Copyright: Anthony Ayiomamitis (TWAN)

Explanation: Reddened by scattered sunlight, the Moon in the center is passing through the center of Earth’s dark umbral shadow in this July 27 lunar eclipse sequence. Left to right the three images are from the start, maximum, and end to 103 minutes of totality from the longest lunar eclipse of the 21st century. The longest path the Moon can follow through Earth’s shadow does cross the shadow’s center, that’s what makes such central lunar eclipses long ones. But July 27 was also the date of lunar apogee, and at the most distant part of its elliptical orbit the Moon moves slowest. For the previous lunar eclipse, last January 31, the Moon was near its orbital perigee. Passing just south of the Earth shadow central axis, totality lasted only 76 minutes. Coming up on January 21, 2019, a third consecutive total lunar eclipse will also be off center and find the Moon near perigee. Then totality will be a mere 62 minutes long.

∞ Source: apod.nasa.gov/apod/ap180803.html


Камни похожие на дольмены Австралия

Australia. Girraween National Park. Камни дольмены в национальном парке



Камни похожие на дольмены Австралия

Australia. Girraween National Park. Камни дольмены в национальном парке



The Granaries and the Commander’s House, Hardknott Roman Fort,…

The Granaries and the Commander’s House, Hardknott Roman Fort, Cumbria, 31.7.18.

The granaries in this location would have been of significant importance and are represented by two rectangular blocks with central columns. (Images 1 to 5).

The Commander’s House foundations are only partially intact and the building was likely shaped in a single storey Mediterranean courtyard and colonnade design. (Images 6 to 8)

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NASA’s TESS Spacecraft Starts Science Operations

NASA – Tess Mission logo.

August 2, 2018

NASA’s Transiting Exoplanet Survey Satellite has started its search for planets around nearby stars, officially beginning science operations on July 25, 2018. TESS is expected to transmit its first series of science data back to Earth in August, and thereafter periodically every 13.5 days, once per orbit, as the spacecraft makes it closest approach to Earth. The TESS Science Team will begin searching the data for new planets immediately after the first series arrives.

Image above: An artist’s illustration of the Transiting Exoplanet Survey Satellite. Image Credits: NASA’s Goddard Space Flight Center.

“I’m thrilled that our new planet hunter mission is ready to start scouring our solar system’s neighborhood for new worlds,” said Paul Hertz, NASA Astrophysics division director at Headquarters, Washington. “Now that we know there are more planets than stars in our universe, I look forward to the strange, fantastic worlds we’re bound to discover.”

TESS is NASA’s latest satellite to search for planets outside our solar system, known as exoplanets. The mission will spend the next two years monitoring the nearest and brightest stars for periodic dips in their light. These events, called transits, suggest that a planet may be passing in front of its star. TESS is expected to find thousands of planets using this method, some of which could potentially support life.

How NASA’s Newest Planet Hunter Scans the Sky

Video above: Animation showing how TESS will observe the sky. TESS will watch each observation sector for at least 27 days, before rotating to the next one, covering first the southern then the northern hemisphere to build a map of 85 percent of the sky. Video Credits: NASA’s Goddard Space Flight Center.

TESS is a NASA Astrophysics Explorer mission led and operated by MIT in Cambridge, Massachusetts, and managed by NASA’s Goddard Space Flight Center in Greenbelt, Maryland. Dr. George Ricker of MIT’s Kavli Institute for Astrophysics and Space Research serves as principal investigator for the mission. Additional partners include Northrop Grumman, based in Falls Church, Virginia; NASA’s Ames Research Center in California’s Silicon Valley; the Harvard-Smithsonian Center for Astrophysics in Cambridge, Massachusetts; MIT’s Lincoln Laboratory in Lexington, Massachusetts; and the Space Telescope Science Institute in Baltimore. More than a dozen universities, research institutes and observatories worldwide are participants in the mission.

For the latest updates on TESS, visit https://www.nasa.gov/tess

Image (mentioned), Video (mentioned), Text, Credits: NASA/Rob Garner/Goddard Space Flight Center/Claire Saravia.

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https://t.co/hvL60wwELQ — XissUFOtoday Space (@xufospace) August 3, 2021 Жаждущий ежик наслаждается пресной водой после нескольких дней в о...