WR 124
| Doppelstern WR 124 | |||||||||
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| Wolf-Rayet-Stern WR-124 mit umgebendem planetarischen Nebel M1-67 (Aufnahme des Hubble-Teleskops) | |||||||||
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| AladinLite | |||||||||
| Beobachtungsdaten Äquinoktium: J2000.0, Epoche: J2000.0 | |||||||||
| Sternbild | Pfeil | ||||||||
| Rektaszension | 19h 11m 30,88s [1] | ||||||||
| Deklination | +16° 51′ 38,2″ [1] | ||||||||
| Helligkeiten | |||||||||
| Scheinbare Helligkeit | 11,17 bis 11,25 mag [2] | ||||||||
| Spektrum und Indices | |||||||||
| Veränderlicher Sterntyp | ELL/WR[2] | ||||||||
| Spektralklasse | WN8 [2] | ||||||||
| Astrometrie | |||||||||
| Radialgeschwindigkeit | (190,0 ± 7,4) km/s | ||||||||
| Parallaxe | (0,12 ± 0,04) mas [1] | ||||||||
| Entfernung | (11000 ± 2000) Lj (3350 ± 670) pc [3] | ||||||||
| Visuelle Absolute Helligkeit Mvis | (−5,3 +0,4−0,5) mag [3] | ||||||||
| Eigenbewegung [1] | |||||||||
| Rek.-Anteil: | (−2,65 ± 0,05) mas/a | ||||||||
| Dekl.-Anteil: | (−5,53 ± 0,05) mas/a | ||||||||
| Physikalische Eigenschaften | |||||||||
| Masse | (9,0 ± 2,5) M☉ [3] | ||||||||
| Radius | (10,1 +2,8−2,6) R☉ [3] | ||||||||
| Leuchtkraft | |||||||||
| Effektive Temperatur | (35800 ± 2000) K [3] | ||||||||
| Alter | 8,6 Mio. a [3] | ||||||||
| Andere Bezeichnungen und Katalogeinträge | |||||||||
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WR 124 (auch QR Sge oder Hen 2-427 genannt)[4] ist ein Riesenstern im Sternbild Pfeil und einer der seltenen Wolf-Rayet-Sterne mit einer Oberflächentemperatur von 35.000 K. Der mehr als 10.000 Lichtjahre von der Erde entfernte Stern besitzt eine scheinbare Helligkeit von 11,2 mag. Der extreme Sternwind, der von ihm ausgeht, treibt seit etwa 10.000 Jahren seine Hülle mit hoher Geschwindigkeit von ihm weg und erzeugt so einen zirkumstellaren Nebel mit der Bezeichnung M1-67 um ihn herum.
(c) NASA, ESA, CSA, STScI, Webb ERO Production Team, CC BY 4.0Infrarotaufnahme mithilfe des James Webb-Weltraumteleskops
Aufnahme mittels Very Large Telescope
Weblinks
- astronews: Bild des Tages 18. August 2015
- A cosmic couple
- James Webb Telescope
Einzelnachweise
- ↑ a b c Hen 2-427. In: SIMBAD. Centre de Données astronomiques de Strasbourg, abgerufen am 11. September 2018.
- ↑ a b c QR Sge. In: VSX. AAVSO, abgerufen am 11. September 2018.
- ↑ a b c d e f g S. V. Marchenko, A. F. J. Moffat, P. A. Crowther: Population I Wolf-Rayet Runaway Stars: The Case of Wr124 and Its Expanding Nebula M1-67. In: The Astrophysical Journal. 724. Jahrgang, 2010, S. L90, doi:10.1088/2041-8205/724/1/L90, arxiv:1011.0785, bibcode:2010ApJ...724L..90M.
- ↑ WHO'S WHO ? ( vom 14. Juni 2007 im Internet Archive)
Auf dieser Seite verwendete Medien
Opaque red circle
Autor/Urheber: IAU and Sky & Telescope magazine (Roger Sinnott & Rick Fienberg), Lizenz: CC BY 3.0
IAU Sagitta chart
Autor/Urheber: ESO, Lizenz: CC BY 4.0
M1-67 is the youngest wind-nebula around a Wolf-Rayet star, called WR124, in our Galaxy. These Wolf-Rayet stars start their lives with dozens of times the mass of our Sun, but loose most of it through a powerful wind, which is ultimately responsible for the formation of the nebula.
Ten years ago, Hubble Space Telescope observations revealed a wealth of small knots and substructures inside the nebula. The same team, led by Cédric Foellmi (ESO), has now used ESO's Very Large Telescope (VLT) to watch how these structures have evolved and what they can teach us about stellar winds, their chemistry, and how they mix with the surrounding interstellar medium, before the star will eventually blow everything away in a fiery supernova explosion.
The image is based on FORS1 data obtained by the Paranal Science team with the VLT through 2 wide (B and V) and 3 narrow-band filters._(weic2307a).jpeg)
(c) NASA, ESA, CSA, STScI, Webb ERO Production Team, CC BY 4.0
The luminous, hot star Wolf-Rayet 124 (WR 124) is prominent at the centre of the NASA/ESA/CSA James Webb Space Telescope’s composite image combining near-infrared and mid-infrared wavelengths of light. The star displays the characteristic diffraction spikes of Webb’s Near-infrared Camera (NIRCam), caused by the physical structure of the telescope itself. NIRCam effectively balances the brightness of the star with the fainter gas and dust surrounding it, while Webb’s Mid-Infrared Instrument (MIRI) reveals the nebula’s structure.Background stars and galaxies populate the field of view and peek through the nebula of gas and dust that has been ejected from the ageing massive star to span 10 light-years across space. A history of the star’s past episodes of mass loss can be read in the nebula’s structure. Rather than smooth shells, the nebula is formed from random, asymmetric ejections. Bright clumps of gas and dust appear like tadpoles swimming toward the star, their tails streaming out behind them, blown back by the stellar wind.This image combines various filters from both Webb imaging instruments, with the colour red assigned to wavelengths of 4.44, 4.7, 12.8, and 18 microns (F444W, F470N, F1280W, F1800W), green to 2.1, 3.35, and 11.3 microns (F210M, F335M, F1130W), and blue to 0.9, 1.5, and 7.7 microns (F090W, F150W, F770W).[Image Description: A large, bright star shines from the centre with smaller stars scattered throughout the image. A clumpy cloud of material surrounds the central star, with more material above and below than on the sides, in some places allowing background stars to peek through. The cloud material is yellow closer to the star.]
Autor/Urheber: Judy Schmidt, Lizenz: CC0
The nebula M1-67 surrounds exploding star Wolf-Rayet 124. From the Hubble Legacy Archive. Processing by Judy Schmidt. Please see this HubbleSite release for further information about this object. http://hubblesite.org/newscenter/archive/releases/1998/38/image/a/
The image is improvement by filling in the blank corner with the single channel of H-alpha data available. Further, the purple stars are tuned to white.
This nebula glows brightly in H-alpha, other channel do not contribute much to it. The three filters used were f675w, f656n, and f555w. The wideband filters were useful for making the stars visible.
Data from Anthony Moffat's proposals, <a href="http://archive.stsci.edu/proposal_search.php?mission=hst&id=6787" rel="nofollow">6787</a> and <a href="http://archive.stsci.edu/proposal_search.php?mission=hst&id=11137" rel="nofollow">11137</a>, were used.
North is NOT up. It is 131.4° counter-clockwise from up.