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Astronomy Picture of the Day
Astronomy Picture of the Day
@apod@reentry.codl.fr  ·  activity timestamp yesterday

Red Spider Planetary Nebula from Webb
Image Credit: ESA/Webb, NASA & CSA, J. H. Kastner (RIT)

Explanation: Oh what a tangled web a planetary nebula can weave. The Red Spider Planetary Nebula shows the complex structure that can result when a normal star ejects its outer gases and becomes a white dwarf star. Officially tagged NGC 6537, this two-lobed symmetric planetary nebula houses one of the hottest white dwarfs ever observed, probably as part of a binary star system. Internal winds flowing out from the central stars, have been measured in excess of 1,000 kilometers per second. These winds expand the nebula, flow along the nebula's walls, and cause waves of hot gas and dust to collide. Atoms caught in these colliding shocks radiate light shown in the featured false-color infrared picture by the James Webb Space Telescope. The Red Spider Nebula lies toward the constellation of the Archer (Sagittarius). Its distance is not well known but has been estimated by some to be about 4,000 light-years.

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A dense starfield surrounds a blue and red nebula that stretches from the lower left to the upper right. The outer parts of the nebula are blue and filamentary, while the innermost part is red and bright.
A dense starfield surrounds a blue and red nebula that stretches from the lower left to the upper right. The outer parts of the nebula are blue and filamentary, while the innermost part is red and bright.
A dense starfield surrounds a blue and red nebula that stretches from the lower left to the upper right. The outer parts of the nebula are blue and filamentary, while the innermost part is red and bright.
Sorry, no caption provided by author
Sorry, no caption provided by author
Sorry, no caption provided by author

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The central star of the Planetary Nebula NGC 6537

The fact that Space Telescope WFPC2 images of the planetary nebula NGC 6537 fail to show the central star is used to derive a limit to its magnitude: it is fainter than a magnitude of 22.4 in the visible. This is used to derive a lower limit to the temperature of the star. The Zanstra temperature is at least 500 000 K. The Energy Balance temperature is found to be consistent with this value, as is the ionization state of the nebula. Assuming a reasonable range of distances for the nebula, the radius of the star can be found. It is consistent with the mass-radius relation of a white dwarf of 0.9 Msun or higher.
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Joel Kastner | RITRIT Logo with TextRIT logoRIT logo and full name (footer)

Joel Kastner, Professor, Imaging Science, Chester F. Carlson Center for Imaging Science, College of Science, 585-475-7179, jhkpci@rit.edu. Joel Kastner (Ph.D. in Astronomy, UCLA 1990) is a Professor on the faculty of Rochester Institute of Technology’s Center for Imaging Science and School of Physics & Astronomy. He was the founding Director of RIT's Laboratory for Multiwavelength Astrophysics.Prior to his two decades at RIT, Prof. Kastner spent almost a decade at MIT, first as Bantrell Postdoc at MIT Haystack Radio Observatory and then as staff scientist with MIT's side of the Chandra (then AXAF) X-ray Science Center.Prof. Kastner's research interests lie in the early and late stages of stellar evolution -- i.e., the formative stages of stars and planetary systems, and their death throes. He has conducted observations of forming and dying stars and stellar systems across a broad swath of the electromagnetic spectrum, from radio to X-rays.Prof. Kastner was among the original group of (roughly 230) astronomers named as "Legacy" Fellows of the American Astronomical Society in 2020, and presently serves as Chair of the AAS Committee on Employment.A complete list of Prof. Kastner's publications can be found at this link to NASA's Astrophysics Data System.

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