NO Aurigae

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NO Aurigae
Auriga constellation map.svg
Red circle.svg
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]
Distance approx. 3,500  ly
(approx. 1,100  pc)
Absolute magnitude  (MV)−5.88 [2]
Details
Mass 4.93 [7]   M☉
Radius 269 [8]   R☉
Luminosity 9,075 [8]   L☉
Surface gravity (log g)−0.037 [8]   cgs
Temperature 3,435 [8]   K
Other designations
BD+31°1049, HD  37536, HIP  26718, HR  1939, SAO  58322
Database references
SIMBAD data
Data sources:
Hipparcos Catalogue,
CCDM (2002),
Bright Star Catalogue (5th rev. ed.)

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.

Contents

Variability

A light curve for NO Aurigae plotted from Hipparcos data NOAurLightCurve.png
A light curve for NO Aurigae plotted from Hipparcos data

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]

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References

  1. 1 2 3 4 5 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. 1 2 3 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. 1 2 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. 1 2 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. 1 2 3 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. 1 2 3 4 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. 1 2 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. 1 2 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. 1 2 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.
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