astro.wikisort.org - StarGD 66 or V361 Aurigae is a 0.64 solar mass (M☉)[4] pulsating white dwarf star located 170 light years from Earth[3] in the Auriga constellation. The estimated cooling age of the white dwarf is 500 million years.[4] Models of the relationship between the initial mass of a star and its final mass as a white dwarf star suggest that when the star was on the main sequence it had a mass of approximately 2.5 M☉, which implies its lifetime was around 830 million years.[4] The total age of the star is thus estimated to be in the range 1.2 to 1.7 billion years.[4]
Star in the constellation Auriga
GD 66
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Observation data Epoch J2000 Equinox J2000 |
Constellation |
Auriga |
Right ascension |
05h 20m 38.31s[2] |
Declination |
+30° 48′ 24.1″[2] |
Apparent magnitude (V) |
15.56[2] |
Characteristics |
Spectral type |
DA[2] |
U−B color index |
-0.59[citation needed] |
B−V color index |
0.22[2] |
Variable type |
Pulsating white dwarf |
Astrometry |
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Proper motion (μ) | RA: 54[2] mas/yr Dec.: −120[2] mas/yr |
Distance | 170[3] ly (51 pc) |
Absolute magnitude (MV) | 12 |
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Details |
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Mass | 0.64 ± 0.03[4] M☉ |
Surface gravity (log g) | 8.05[5] cgs |
Temperature | 11980[5] K |
Age | 1.2–1.7 billion[4] years |
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Other designations |
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V361 Aurigae, GD 66, 2MASS J05203829+3048239, WD 0517+30, EGGR 572, WD 0517+307 |
Database references |
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SIMBAD | data |
The star is a pulsating white dwarf of type DAV, with an extremely stable period. Small variations in the phase of pulsation led to the suggestion that the star was being orbited by a giant planet which caused the pulsations to be delayed due to the varying distance to the star caused by the reflex motion about the system's centre-of-mass.[3] Observations with the Spitzer Space Telescope failed to directly detect the planet, which put an upper limit on the mass of 5–6 Jupiter masses.[4] Investigation of a separate pulsation mode revealed timing variations in antiphase with the variations in the originally-analysed pulsation mode.[6] This would not be the case if the variations were caused by an orbiting planet, and thus the timing variations must have a different cause. This illustrates the potential dangers of attempting to detect planets by white dwarf pulsation timing.[7]
References
- Fontaine, G.; Wesemael, F.; Bergeron, P.; Lacombe, P.; Lamontagne, R. (July 1985). "The demise of mode identification in the pulsating DA white dwarf GD 66". The Astrophysical Journal. 294: 339–344. doi:10.1086/163301. Retrieved 2 November 2021.
- "V* V361 Aur". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2008-12-19.
- Mullally, F.; et al. (2008). "Limits on Planets around Pulsating White Dwarf Stars". The Astrophysical Journal. 676 (1): 573–583. arXiv:0801.3104. Bibcode:2008ApJ...676..573M. doi:10.1086/528672.
- Mullally, F.; et al. (2009). "Spitzer Planet Limits around the Pulsating White Dwarf GD66". The Astrophysical Journal. 694: 327–331. arXiv:0812.2951. Bibcode:2009ApJ...694..327M. doi:10.1088/0004-637X/694/1/327. S2CID 16241754.
- Bergeron, P.; et al. (2004). "On the Purity of the ZZ Ceti Instability Strip: Discovery of More Pulsating DA White Dwarfs on the Basis of Optical Spectroscopy". The Astrophysical Journal. 600 (1): 404–408. arXiv:astro-ph/0309483. Bibcode:2004ApJ...600..404B. doi:10.1086/379808. S2CID 16636294.
- Hermes, James J. (2013). Complications to the Planetary Hypothesis for GD 66. AAS Meeting #221. American Astronomical Society. Bibcode:2013AAS...22142404H.
- Hermes, J. J. (2012). 8 Years On: A Search for Planets Around Isolated White Dwarfs (PDF). Planets around Stellar Remnants. Archived from the original (PDF) on 2014-12-27.
External links
Constellation of Auriga |
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Stars | |
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Nebulae | |
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 Category |
На других языках
- [en] GD 66
[es] GD 66
GD 66 es una estrella enana blanca con una masa de un 64% la del Sol, que se encuentra a 166 años luz de distancia.[2]
[ru] GD 66
V361 Возничего (лат. V361 Aurigae), GD 66 — одиночная переменная звезда в созвездии Возничего на расстоянии приблизительно 187 световых лет (около 57,2 парсеков) от Солнца. Видимая звёздная величина звезды — от +15,62m до +15,6m[7].
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