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| Ultimi commenti - The Universe in Super Definition |
Kepler_10b-PIA13776.jpgExo-Planet "Kepler 10b"152 visiteCaption NASA:"Artist's concept of the first rocky world discovered by NASA's Kepler Mission. The Planet, called Kepler 10-b, is shown in front of its Host (Parent) Star".MareKromium06/19/20 at 21:03Anakin: ah! quindi tu dici che a queste distanze un sistem...
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Kepler_10b-PIA13776.jpgExo-Planet "Kepler 10b"152 visiteCaption NASA:"Artist's concept of the first rocky world discovered by NASA's Kepler Mission. The Planet, called Kepler 10-b, is shown in front of its Host (Parent) Star".MareKromium06/19/20 at 16:43MareKromium: No Anakin. E' che noi vediamo i "Sistemi ...
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Kepler_10b-PIA13776.jpgExo-Planet "Kepler 10b"152 visiteCaption NASA:"Artist's concept of the first rocky world discovered by NASA's Kepler Mission. The Planet, called Kepler 10-b, is shown in front of its Host (Parent) Star".MareKromium06/17/20 at 07:12Anakin: Fino ad ora sono stati trovati diversi sistemi sol...
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EpsilonEridani-PIA11375.jpgEpsilon Eridani56 visiteThis artist's conception shows the closest known Planetary System to our own, called Epsilon Eridani. Observations from NASA's Spitzer Space Telescope show that the system hosts two Asteroid Belts, in addition to previously identified candidate planets and an outer Comet Ring.
Epsilon Eridani is located about 10 LY away in the constellation Eridanus. It is visible in the night skies with the naked eye.
The System's Inner Asteroid Belt appears as the yellowish ring around the star, while the Outer Asteroid Belt is in the foreground. The outermost Comet Ring is too far out to be seen in this view, but comets originating from it are shown in the upper right corner.
Astronomers think that each of Epsilon Eridani's Asteroid Belts could have a planet orbiting just outside it, shepherding its rocky debris into a ring in the same way that Jupiter helps keep our asteroid belt confined.
The planet near the inner belt was previously identified in 2000 via the radial velocity, or "star wobble", technique, while the planet near the outer belt was inferred when Spitzer discovered the belt.
The inner belt orbits at a distance of about 3 AU from its star — or about the same position as the Asteroid Belt in our own Solar System (an astronomical unit is the distance between Earth and the Sun). The second Asteroid Belt lies at about 20 AU from the star, or a position comparable to Uranus in our Solar System.
The outer Comet Ring orbits from 35 to 90 AU from the star; our Solar System's analogous Kuiper Belt extends from about 30 to 50 AU from the sun.MareKromium03/26/20 at 17:49MareKromium: L'"Oggetto" ? estremamente veloce e ...
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EpsilonEridani-PIA11375.jpgEpsilon Eridani56 visiteThis artist's conception shows the closest known Planetary System to our own, called Epsilon Eridani. Observations from NASA's Spitzer Space Telescope show that the system hosts two Asteroid Belts, in addition to previously identified candidate planets and an outer Comet Ring.
Epsilon Eridani is located about 10 LY away in the constellation Eridanus. It is visible in the night skies with the naked eye.
The System's Inner Asteroid Belt appears as the yellowish ring around the star, while the Outer Asteroid Belt is in the foreground. The outermost Comet Ring is too far out to be seen in this view, but comets originating from it are shown in the upper right corner.
Astronomers think that each of Epsilon Eridani's Asteroid Belts could have a planet orbiting just outside it, shepherding its rocky debris into a ring in the same way that Jupiter helps keep our asteroid belt confined.
The planet near the inner belt was previously identified in 2000 via the radial velocity, or "star wobble", technique, while the planet near the outer belt was inferred when Spitzer discovered the belt.
The inner belt orbits at a distance of about 3 AU from its star — or about the same position as the Asteroid Belt in our own Solar System (an astronomical unit is the distance between Earth and the Sun). The second Asteroid Belt lies at about 20 AU from the star, or a position comparable to Uranus in our Solar System.
The outer Comet Ring orbits from 35 to 90 AU from the star; our Solar System's analogous Kuiper Belt extends from about 30 to 50 AU from the sun.MareKromium03/26/20 at 07:12Anakin: non si sa, eppure in quel punto c'? qualcosa c...
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EpsilonEridani-PIA11375.jpgEpsilon Eridani56 visiteThis artist's conception shows the closest known Planetary System to our own, called Epsilon Eridani. Observations from NASA's Spitzer Space Telescope show that the system hosts two Asteroid Belts, in addition to previously identified candidate planets and an outer Comet Ring.
Epsilon Eridani is located about 10 LY away in the constellation Eridanus. It is visible in the night skies with the naked eye.
The System's Inner Asteroid Belt appears as the yellowish ring around the star, while the Outer Asteroid Belt is in the foreground. The outermost Comet Ring is too far out to be seen in this view, but comets originating from it are shown in the upper right corner.
Astronomers think that each of Epsilon Eridani's Asteroid Belts could have a planet orbiting just outside it, shepherding its rocky debris into a ring in the same way that Jupiter helps keep our asteroid belt confined.
The planet near the inner belt was previously identified in 2000 via the radial velocity, or "star wobble", technique, while the planet near the outer belt was inferred when Spitzer discovered the belt.
The inner belt orbits at a distance of about 3 AU from its star — or about the same position as the Asteroid Belt in our own Solar System (an astronomical unit is the distance between Earth and the Sun). The second Asteroid Belt lies at about 20 AU from the star, or a position comparable to Uranus in our Solar System.
The outer Comet Ring orbits from 35 to 90 AU from the star; our Solar System's analogous Kuiper Belt extends from about 30 to 50 AU from the sun.MareKromium03/24/20 at 17:47walthari: ma che è??? Un'astronave madre?????
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EpsilonEridani-PIA11375.jpgEpsilon Eridani56 visiteThis artist's conception shows the closest known Planetary System to our own, called Epsilon Eridani. Observations from NASA's Spitzer Space Telescope show that the system hosts two Asteroid Belts, in addition to previously identified candidate planets and an outer Comet Ring.
Epsilon Eridani is located about 10 LY away in the constellation Eridanus. It is visible in the night skies with the naked eye.
The System's Inner Asteroid Belt appears as the yellowish ring around the star, while the Outer Asteroid Belt is in the foreground. The outermost Comet Ring is too far out to be seen in this view, but comets originating from it are shown in the upper right corner.
Astronomers think that each of Epsilon Eridani's Asteroid Belts could have a planet orbiting just outside it, shepherding its rocky debris into a ring in the same way that Jupiter helps keep our asteroid belt confined.
The planet near the inner belt was previously identified in 2000 via the radial velocity, or "star wobble", technique, while the planet near the outer belt was inferred when Spitzer discovered the belt.
The inner belt orbits at a distance of about 3 AU from its star — or about the same position as the Asteroid Belt in our own Solar System (an astronomical unit is the distance between Earth and the Sun). The second Asteroid Belt lies at about 20 AU from the star, or a position comparable to Uranus in our Solar System.
The outer Comet Ring orbits from 35 to 90 AU from the star; our Solar System's analogous Kuiper Belt extends from about 30 to 50 AU from the sun.MareKromium03/20/20 at 13:58Anakin: Se non lo avete fatto, vi invito a guardare questo...
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YoungStar-PIA09266.jpgThe "O"-Star68 visite"The further on the edge, the hotter the intensity," sings Kenny Loggins in "Danger Zone," a song made famous by the movie "Top Gun." The same words ring true for young, cooler stars like our sun that live in the danger zones around scorching hot stars, called O-stars. The closer a young, maverick star happens to be to a super hot O-star, the more likely its burgeoning planets will be blasted into space.
This artist's animation illustrates how this process works. The movie begins by showing an O-star in a murky star-forming region. It then pans out to show a young, cooler star and its swirling disk of planet-forming material. Disks like this one, called protoplanetary disks, are where planets are born. Gas and dust in a disk clumps together into tiny balls that sweep through the material, growing in size to eventually become full-grown planets.
The young star happens to lie within the "danger zone" around the O-star, which means that it is too close to the hot star to keep its disk. Radiation and winds from the O-star boil and blow away the material, respectively. This process, called photoevaporation, is sped up here but takes anywhere from 100,000 to about 1,000,000 years. Without a disk, the young star will not be able to produce planets.
Our own sun and its suite of planets might have grown up on the edge of an O-star's danger zone before migrating to its current, spacious home. However, we know that our young sun didn't linger for too long in any hazardous territory, or our planets, and life, wouldn't be here today.
NASA's Spitzer Space Telescope surveyed the danger zones around five O-stars in the Rosette nebula. It was able to determine that the zones are spheres with a radius of approximately 1.6 light-years, or 10 trillion miles.
MareKromium02/19/20 at 11:23walthari: un abbraccio Paolo
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YoungStar-PIA09266.jpgThe "O"-Star68 visite"The further on the edge, the hotter the intensity," sings Kenny Loggins in "Danger Zone," a song made famous by the movie "Top Gun." The same words ring true for young, cooler stars like our sun that live in the danger zones around scorching hot stars, called O-stars. The closer a young, maverick star happens to be to a super hot O-star, the more likely its burgeoning planets will be blasted into space.
This artist's animation illustrates how this process works. The movie begins by showing an O-star in a murky star-forming region. It then pans out to show a young, cooler star and its swirling disk of planet-forming material. Disks like this one, called protoplanetary disks, are where planets are born. Gas and dust in a disk clumps together into tiny balls that sweep through the material, growing in size to eventually become full-grown planets.
The young star happens to lie within the "danger zone" around the O-star, which means that it is too close to the hot star to keep its disk. Radiation and winds from the O-star boil and blow away the material, respectively. This process, called photoevaporation, is sped up here but takes anywhere from 100,000 to about 1,000,000 years. Without a disk, the young star will not be able to produce planets.
Our own sun and its suite of planets might have grown up on the edge of an O-star's danger zone before migrating to its current, spacious home. However, we know that our young sun didn't linger for too long in any hazardous territory, or our planets, and life, wouldn't be here today.
NASA's Spitzer Space Telescope surveyed the danger zones around five O-stars in the Rosette nebula. It was able to determine that the zones are spheres with a radius of approximately 1.6 light-years, or 10 trillion miles.
MareKromium02/19/20 at 09:40Anakin: Grande abbraccio. Ti aspettiamo
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YoungStar-PIA09266.jpgThe "O"-Star68 visite"The further on the edge, the hotter the intensity," sings Kenny Loggins in "Danger Zone," a song made famous by the movie "Top Gun." The same words ring true for young, cooler stars like our sun that live in the danger zones around scorching hot stars, called O-stars. The closer a young, maverick star happens to be to a super hot O-star, the more likely its burgeoning planets will be blasted into space.
This artist's animation illustrates how this process works. The movie begins by showing an O-star in a murky star-forming region. It then pans out to show a young, cooler star and its swirling disk of planet-forming material. Disks like this one, called protoplanetary disks, are where planets are born. Gas and dust in a disk clumps together into tiny balls that sweep through the material, growing in size to eventually become full-grown planets.
The young star happens to lie within the "danger zone" around the O-star, which means that it is too close to the hot star to keep its disk. Radiation and winds from the O-star boil and blow away the material, respectively. This process, called photoevaporation, is sped up here but takes anywhere from 100,000 to about 1,000,000 years. Without a disk, the young star will not be able to produce planets.
Our own sun and its suite of planets might have grown up on the edge of an O-star's danger zone before migrating to its current, spacious home. However, we know that our young sun didn't linger for too long in any hazardous territory, or our planets, and life, wouldn't be here today.
NASA's Spitzer Space Telescope surveyed the danger zones around five O-stars in the Rosette nebula. It was able to determine that the zones are spheres with a radius of approximately 1.6 light-years, or 10 trillion miles.
MareKromium02/18/20 at 18:17Ufologo: Quindi, un saluto siderale con relativo abbraccio!
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YoungStar-PIA09266.jpgThe "O"-Star68 visite"The further on the edge, the hotter the intensity," sings Kenny Loggins in "Danger Zone," a song made famous by the movie "Top Gun." The same words ring true for young, cooler stars like our sun that live in the danger zones around scorching hot stars, called O-stars. The closer a young, maverick star happens to be to a super hot O-star, the more likely its burgeoning planets will be blasted into space.
This artist's animation illustrates how this process works. The movie begins by showing an O-star in a murky star-forming region. It then pans out to show a young, cooler star and its swirling disk of planet-forming material. Disks like this one, called protoplanetary disks, are where planets are born. Gas and dust in a disk clumps together into tiny balls that sweep through the material, growing in size to eventually become full-grown planets.
The young star happens to lie within the "danger zone" around the O-star, which means that it is too close to the hot star to keep its disk. Radiation and winds from the O-star boil and blow away the material, respectively. This process, called photoevaporation, is sped up here but takes anywhere from 100,000 to about 1,000,000 years. Without a disk, the young star will not be able to produce planets.
Our own sun and its suite of planets might have grown up on the edge of an O-star's danger zone before migrating to its current, spacious home. However, we know that our young sun didn't linger for too long in any hazardous territory, or our planets, and life, wouldn't be here today.
NASA's Spitzer Space Telescope surveyed the danger zones around five O-stars in the Rosette nebula. It was able to determine that the zones are spheres with a radius of approximately 1.6 light-years, or 10 trillion miles.
MareKromium02/18/20 at 17:36MareKromium: Amici, mi assento qualche giorno. Domani ho un imp...
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IC-348-PIA12210.jpgCreation...104 visiteThis artist's conception shows a lump of material in a swirling, planet- forming disk. Astronomers using NASA's Spitzer Space Telescope found evidence that a companion to a star -- either another star or a planet -- could be pushing planetary material together, as illustrated here.
Planets are born out of spinning disks of gas and dust. They can carve out lanes or gaps in the disks as they grow bigger and bigger. Scientists used Spitzer's infrared vision to study the disk around a star called LRLL 31, located about 1000 LY away in the IC 348 Region of the constellation Perseus. Spitzer's new infrared observations reveal that the disk has both an inner and outer gap.
What's more, the data show that infrared light from the disk is changing over as little time as one week -- a very unusual occurrence. In particular, light of different wavelengths seesawed back and forth, with short-wavelength light going up when long-wavelength light went down, and vice versa.
According to astronomers, this change could be caused by a companion to the star (illustrated as a planet in this picture). As the companion spins around, its gravity would cause the wall of the inner disk to squeeze into a lump. This lump would also spin around the star, shadowing part of the outer disk. When the bright side of the lump is on the far side of the star, and facing Earth, more infrared light at shorter wavelengths should be observed (hotter material closer to the star emits shorter wavelengths of infrared light). In addition, the shadow of the lump should cause longer-wavelength infrared light from the outer disk to decrease. The opposite would be true when the lump is in front of the star and its bright side is hidden (shorter-wavelength light would go down, and longer- wavelength light up). This is precisely what Spitzer observed.
The size of the lump and the planet have been exaggerated to better illustrate the dynamics of the system.MareKromium08/03/16 at 20:37Ivana Tognoloni: forse è in vacanza....
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