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NO Aurigae is a pulsating variable star in the constellation Auriga. It is an unusually-luminous asymptotic giant branch star about 3,500 light years away.

NO Aurigae
Location of NO Aurigae (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Auriga
Right ascension 05h 40m 42.050s[1]
Declination +31° 55′ 14.20″[1]
Apparent magnitude (V) 6.21[2] (6.06 - 6.44[3])
Characteristics
Evolutionary stage Asymptotic giant branch[4]
Spectral type M2S Iab[3]
U−B color index +2.22[5]
B−V color index +2.09[5]
R−I color index +1.41[5]
Variable type LC[3]
Astrometry
Radial velocity (Rv)7.21±0.45[6] km/s
Proper motion (μ) RA: 0.061±0.093[1] mas/yr
Dec.: −2.959±0.051[1] mas/yr
Parallax (π)0.9189 ± 0.0930 mas[1]
Distanceapprox. 3,500 ly
(approx. 1,100 pc)
Absolute magnitude (MV)−5.88[2]
Details
Mass4.93[7] M☉
Radius269[8] R☉
Luminosity9,075[8] L☉
Surface gravity (log g)−0.037[8] cgs
Temperature3,435[8] K
Other designations
BD+31°1049, HD 37536, HIP 26718, HR 1939, SAO 58322
Database references
SIMBADdata
Data sources:
Hipparcos Catalogue,
CCDM (2002),
Bright Star Catalogue (5th rev. ed.)

Variability


A light curve for NO Aurigae plotted from Hipparcos data[9]
A light curve for NO Aurigae plotted from Hipparcos data[9]

NO Aurigae is listed in the General Catalogue of Variable Stars as a slow irregular variable, indicating that no regularity could be found in the brightness variations. Other studies have suggested possible periods of 102.1, 173, and 226 days, and would classify it as a semiregular variable star.[10] The maximum visual magnitude range is 6.05–6.50.[10]


Properties


Most studies of NO Aurigae treat it as a supergiant member of the Auriga OB1 stellar association at about 1.4 kpc.[11][12] On this basis it would have a luminosity around 67,000 L☉ and a radius around 630 R☉.[2][11]

NO Aurigae is an MS star, intermediate between spectral type M and S. These are typically Asymptotic Giant Branch stars which can appear with supergiant spectra due to their large size and low mass.[4] Possible detection of Technetium in the spectrum is a symptom of the third dredge-up which occurs only in late AGB stars.[12]


References


  1. Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  2. Levesque, Emily M.; Massey, Philip; Olsen, K. A. G.; Plez, Bertrand; Josselin, Eric; Maeder, Andre; Meynet, Georges (2005). "The Effective Temperature Scale of Galactic Red Supergiants: Cool, but Not As Cool As We Thought". The Astrophysical Journal. 628 (2): 973–985. arXiv:astro-ph/0504337. Bibcode:2005ApJ...628..973L. doi:10.1086/430901. S2CID 15109583.
  3. Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  4. Guandalini, R.; Busso, M. (2008). "Infrared photometry and evolution of mass-losing AGB stars. II. Luminosity and colors of MS and S stars". Astronomy and Astrophysics. 488 (2): 675–684. arXiv:0806.4591. Bibcode:2008A&A...488..675G. doi:10.1051/0004-6361:200809932. S2CID 14294870.
  5. Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D.
  6. Famaey, B.; Jorissen, A.; Luri, X.; Mayor, M.; Udry, S.; Dejonghe, H.; Turon, C. (2005). "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters". Astronomy and Astrophysics. 430: 165. arXiv:astro-ph/0409579. Bibcode:2005A&A...430..165F. doi:10.1051/0004-6361:20041272. S2CID 17804304.
  7. Hohle, M. M.; Neuhäuser, R.; Schutz, B. F. (April 2010). "Masses and luminosities of O- and B-type stars and red supergiants". Astronomische Nachrichten. 331 (4): 349. arXiv:1003.2335. Bibcode:2010AN....331..349H. doi:10.1002/asna.200911355. S2CID 111387483.
  8. McDonald, I.; Zijlstra, A. A.; Watson, R. A. (2017). "Fundamental parameters and infrared excesses of Tycho-Gaia stars". Monthly Notices of the Royal Astronomical Society. 471 (1): 770. arXiv:1706.02208. Bibcode:2017MNRAS.471..770M. doi:10.1093/mnras/stx1433. S2CID 73594365.
  9. "Hipparcos Tools Interactive Data Access". Hipparcos. ESA. Retrieved 8 December 2021.
  10. Watson, C. L. (2006). "The International Variable Star Index (VSX)". The Society for Astronomical Sciences 25th Annual Symposium on Telescope Science. Held May 23–25. 25: 47. Bibcode:2006SASS...25...47W.
  11. Mauron, N.; Josselin, E. (2011). "The mass-loss rates of red supergiants and the de Jager prescription". Astronomy and Astrophysics. 526: A156. arXiv:1010.5369. Bibcode:2011A&A...526A.156M. doi:10.1051/0004-6361/201013993. S2CID 119276502.
  12. Josselin, E.; Plez, B. (2007). "Atmospheric dynamics and the mass loss process in red supergiant stars". Astronomy and Astrophysics. 469 (2): 671. arXiv:0705.0266. Bibcode:2007A&A...469..671J. doi:10.1051/0004-6361:20066353. S2CID 17789027.



На других языках

- [en] NO Aurigae

[es] NO Aurigae

NO Aurigae (NO Aur / HD 37536 / HR 1939 / HIP 26718)[1] es una estrella variable en la constelación de Auriga de magnitud aparente media +6,24. Aunque se ha señalado su asociación con el cúmulo estelar Aurigae OB1, la paralaje medida por el satélite Hipparcos la sitúa a 1370 años luz del Sistema Solar, un tercio de la distancia a la que se encuentra el cúmulo.[2]

[ru] NO Возничего

NO Возничего (лат. NO Aurigae), HD 37536 — одиночная переменная звезда в созвездии Возничего на расстоянии (вычисленном из значения параллакса) приблизительно 7182 световых лет (около 2202 парсеков) от Солнца. Видимая звёздная величина звезды — от +6,44m до +6,06m[5].


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