#deep_space

Hubble's image of spiral galaxy NGC 6951 shows its bright blue spiral arms, bars, patches of star clusters, and clumps of dust. The galaxy NGC 6951, which lies 78 million light-years from Earth, was captured in a new Hubble image created by the Wide Field Camera (WFC3) and the Advanced Camera for Surveys (ACS). The image shows bright blue spiral arms, star clusters, and a dark orange dust cloud. [caption id="attachment_64740" align="aligncenter" width="780"] spiral galaxy NGC 6951[/caption] The history of this galaxy is quite amazing. About 800 million years ago, NGC 6951 was known for its high rate of star formation, but then star formation stopped for 300 million years. Over the past 25 years, six powerful supernova explosions have occurred, causing the extinction of some of these stars. The average age of a star cluster in the galaxy is between 200 and 300 million years, but some have reached the age of one billion years. An angle straight to the heart: Hubble captured a detailed image of the spiral galaxy NGC 6951 NGC 6951 is classified as a Type II Seyfert galaxy due to its infrared emission and the presence of a slow-moving gaseous environment at the center. However, some astronomers also consider it to be a low-ionization galaxy with an emission line in the core, implying a cooler and less ionized core. Near the center of the galaxy lies a supermassive black hole, which is surrounded by a ring of stars, gas, and dust with a diameter of about 3,700 light years. This ring is also known as the "central ring" and is thought to have star formation for 1 to 1.5 billion years, with 40% of its mass consisting of stars less than 100 million years old. This image of NGC 6951 is part of NASA's Hubble Photo Sharing Campaign, which features new images taken by the space telescope every day from October 2 to October 7.

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.

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.

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.

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