#Hubble_Space_Telescope_successor

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The James Webb Telescope helped observe the disappearance of the disk around the young star SZ Cha Data obtained with the James Webb Space Telescope (JWST) allowed us to draw conclusions about the process of planet formation in gas-dust disks. It turns out that the amount of ionized neon in these disks can serve as an indicator of the rate of planet formation. Previously, astronomers have already observed disks of gas and dust around young stars, but the process of their formation takes a very long time - hundreds of thousands, or even millions of years. It is almost impossible to observe changes in disks over short time intervals. In a new study, James Webb was able to detect changes in one of these disks where planet formation occurs. In observations made by a team led by Catherine Espaillat in 2008 using NASA's Spitzer Telescope, an infrared spectral line associated with doubly ionized neon ([Ne III]) was seen. The signal came from a disk of gas and dust around the young star SZ Chamaeleontis (SZ Cha).  [caption id="attachment_82600" align="alignnone" width="780"] James Webb[/caption] James Webb Helps Find Key to the Rate of Planet Formation When an atom collides with a photon, it becomes "ionized" and "doubly ionized" atoms lose two electrons. In the SZ Cha disk, the amount of doubly ionized neon appears to be very low compared to disks typically exposed to X-ray emission from young stars. The appearance of this neon indicated that the dominant type of radiation in the SZ Cha system was "extreme ultraviolet" (EUV) radiation, capable of destroying gas and dust in the protoplanetary disk, but not as quickly as X-rays. X-ray radiation destroys the protoplanetary disk 100 times faster than ultraviolet radiation. From this we can conclude that the rate of “evaporation” of the disk and, accordingly, the time during which the formation of planets is possible depends on the energy and type of radiation.  In 2023, Espaillat and her team conducted a new long-term observation of the SZ Cha system using JWST's MIRI instrument. The scientists found that the amount of doubly ionized neon was significantly reduced compared to singly ionized neon. Additional observations using ground-based telescopes allow us to study the properties of protoplanetary disks in even more detail. For example, the CHIRON spectrometer on the SMARTS telescope at Cerro Tololo Observatory measured the blueshift of alpha hydrogen from the star SZ Cha. The blue shift is a Doppler-type change that indicates that something is moving toward our detectors, in this case hydrogen. Scientists interpret this phenomenon as a "stellar wind" of particles emanating from the star. This wind is thought to be dense enough to absorb ultraviolet radiation, but still transmits X-rays, indicating the latter's dominance in the evolution of this star system.  The discovery of doubly ionized neon in 2008, but its absence in subsequent observations, supports the assumption of X-ray dominance in the SZ Cha system. Thus, the amount of doubly ionized neon can serve as an indicator of ultraviolet and X-ray radiation affecting the protoplanetary disk. Astronomers can use this value to more accurately determine the time it takes planets to form in such a system before their disk disappears.

[phonemantra-blog]

The James Webb Telescope helped observe the disappearance of the disk around the young star SZ Cha Data obtained with the James Webb Space Telescope (JWST) allowed us to draw conclusions about the process of planet formation in gas-dust disks. It turns out that the amount of ionized neon in these disks can serve as an indicator of the rate of planet formation. Previously, astronomers have already observed disks of gas and dust around young stars, but the process of their formation takes a very long time - hundreds of thousands, or even millions of years. It is almost impossible to observe changes in disks over short time intervals. In a new study, James Webb was able to detect changes in one of these disks where planet formation occurs. In observations made by a team led by Catherine Espaillat in 2008 using NASA's Spitzer Telescope, an infrared spectral line associated with doubly ionized neon ([Ne III]) was seen. The signal came from a disk of gas and dust around the young star SZ Chamaeleontis (SZ Cha).  [caption id="attachment_82600" align="alignnone" width="780"] James Webb[/caption] James Webb Helps Find Key to the Rate of Planet Formation When an atom collides with a photon, it becomes "ionized" and "doubly ionized" atoms lose two electrons. In the SZ Cha disk, the amount of doubly ionized neon appears to be very low compared to disks typically exposed to X-ray emission from young stars. The appearance of this neon indicated that the dominant type of radiation in the SZ Cha system was "extreme ultraviolet" (EUV) radiation, capable of destroying gas and dust in the protoplanetary disk, but not as quickly as X-rays. X-ray radiation destroys the protoplanetary disk 100 times faster than ultraviolet radiation. From this we can conclude that the rate of “evaporation” of the disk and, accordingly, the time during which the formation of planets is possible depends on the energy and type of radiation.  In 2023, Espaillat and her team conducted a new long-term observation of the SZ Cha system using JWST's MIRI instrument. The scientists found that the amount of doubly ionized neon was significantly reduced compared to singly ionized neon. Additional observations using ground-based telescopes allow us to study the properties of protoplanetary disks in even more detail. For example, the CHIRON spectrometer on the SMARTS telescope at Cerro Tololo Observatory measured the blueshift of alpha hydrogen from the star SZ Cha. The blue shift is a Doppler-type change that indicates that something is moving toward our detectors, in this case hydrogen. Scientists interpret this phenomenon as a "stellar wind" of particles emanating from the star. This wind is thought to be dense enough to absorb ultraviolet radiation, but still transmits X-rays, indicating the latter's dominance in the evolution of this star system.  The discovery of doubly ionized neon in 2008, but its absence in subsequent observations, supports the assumption of X-ray dominance in the SZ Cha system. Thus, the amount of doubly ionized neon can serve as an indicator of ultraviolet and X-ray radiation affecting the protoplanetary disk. Astronomers can use this value to more accurately determine the time it takes planets to form in such a system before their disk disappears.

[phonemantra-blog]

The James Webb Telescope helped observe the disappearance of the disk around the young star SZ Cha Data obtained with the James Webb Space Telescope (JWST) allowed us to draw conclusions about the process of planet formation in gas-dust disks. It turns out that the amount of ionized neon in these disks can serve as an indicator of the rate of planet formation. Previously, astronomers have already observed disks of gas and dust around young stars, but the process of their formation takes a very long time - hundreds of thousands, or even millions of years. It is almost impossible to observe changes in disks over short time intervals. In a new study, James Webb was able to detect changes in one of these disks where planet formation occurs. In observations made by a team led by Catherine Espaillat in 2008 using NASA's Spitzer Telescope, an infrared spectral line associated with doubly ionized neon ([Ne III]) was seen. The signal came from a disk of gas and dust around the young star SZ Chamaeleontis (SZ Cha).  [caption id="attachment_82600" align="alignnone" width="780"] James Webb[/caption] James Webb Helps Find Key to the Rate of Planet Formation When an atom collides with a photon, it becomes "ionized" and "doubly ionized" atoms lose two electrons. In the SZ Cha disk, the amount of doubly ionized neon appears to be very low compared to disks typically exposed to X-ray emission from young stars. The appearance of this neon indicated that the dominant type of radiation in the SZ Cha system was "extreme ultraviolet" (EUV) radiation, capable of destroying gas and dust in the protoplanetary disk, but not as quickly as X-rays. X-ray radiation destroys the protoplanetary disk 100 times faster than ultraviolet radiation. From this we can conclude that the rate of “evaporation” of the disk and, accordingly, the time during which the formation of planets is possible depends on the energy and type of radiation.  In 2023, Espaillat and her team conducted a new long-term observation of the SZ Cha system using JWST's MIRI instrument. The scientists found that the amount of doubly ionized neon was significantly reduced compared to singly ionized neon. Additional observations using ground-based telescopes allow us to study the properties of protoplanetary disks in even more detail. For example, the CHIRON spectrometer on the SMARTS telescope at Cerro Tololo Observatory measured the blueshift of alpha hydrogen from the star SZ Cha. The blue shift is a Doppler-type change that indicates that something is moving toward our detectors, in this case hydrogen. Scientists interpret this phenomenon as a "stellar wind" of particles emanating from the star. This wind is thought to be dense enough to absorb ultraviolet radiation, but still transmits X-rays, indicating the latter's dominance in the evolution of this star system.  The discovery of doubly ionized neon in 2008, but its absence in subsequent observations, supports the assumption of X-ray dominance in the SZ Cha system. Thus, the amount of doubly ionized neon can serve as an indicator of ultraviolet and X-ray radiation affecting the protoplanetary disk. Astronomers can use this value to more accurately determine the time it takes planets to form in such a system before their disk disappears.

[phonemantra-blog]

Even earlier The James Webb Space Telescope (JWST) discovered the two most distant galaxies at redshifts 13.079 and 12.393. This discovery supports the Big Bang theory and further confirms the picture of galaxy formation. The discovery was made possible thanks to a gravitational lens played by the galactic cluster Abell 2744, also known as the Pandora Cluster. This cluster is located about 3.5 billion light-years away, and its gravitational field bends the structure of space-time in such a way that it “magnifies” distant galaxies. Using JWST and its ability to probe early galaxies magnified by this gravitational lens, researcher Bingjie Wang of Penn State University and her colleagues in the JWST UNCOVER program were able to discover these two galaxies with the highest redshifts. [caption id="attachment_82136" align="aligncenter" width="650"] James Webb Space[/caption] Cosmological redshift occurs due to the expansion of the Universe. The further away the galaxy, the more the universe expanded as the light from that galaxy traveled through space to reach our detectors. Galaxies that existed just 300 to 400 million years after the Big Bang emit infrared light that is invisible to the human eye but can be observed by the NIRCam camera and JWST's NIRspec spectrometer. The James Webb Space Telescope discovered two unusual distant galaxies The researchers were able to identify enlarged images of these two high-redshift galaxies - UNCOVER-z13 and UNCOVER-z12 (z indicates redshift, which is the letter used in astrophysics). UNCOVER-z13 has a redshift of 13.079, making it the second most distant galaxy known to date. We see it as it was just 330 million years after the Big Bang. The most distant confirmed galaxy, JADES-GS-z13-0, has a redshift of 13.2 JWST discovered it in 2022. The second galaxy, UNCOVER-z12, has a redshift of 12.393 and ranks fourth on the list of most distant galaxies. We see it as it was just 350 million years after the Big Bang. These two galaxies stand out because of their appearance—unlike other galaxies at comparable redshifts, they do not appear as small dots. In contrast, the UNCOVER-z12 galaxy has a disk approximately 2,000 light-years in diameter, six times larger than other galaxies observed during this period. “The two galaxies have very different properties. Their differences will be the subject of further research. We expected that these galaxies are formed from similar materials, but now we see significant differences between them,” noted Bingji Wang. Despite these differences in the properties of the galaxies, both are fully consistent with the Big Bang model, even so early in the Universe. The model explains how, after the creation of the Universe, galaxies slowly grew, merged with other galaxies and gas clouds, and actively formed stars. This growth contributed to an increase in the diversity of elements contained in young galaxies and the introduction of heavy elements - heavier than hydrogen and helium. The galaxies discovered by UNCOVER JWST are young and small, with low concentrations of heavy elements, and are actively forming stars, supporting the Big Bang theory, as noted by Joel Leja, a member of Wang's team. JWST has the ability to detect galaxies at even higher redshifts than UNCOVER-z13 and -z12. But they were not captured by the gravitational lens created by the Pandora Cluster.