Astronomy:NO Aurigae

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Short description: Star in the constellation Auriga
NO Aurigae
Location of NO Aurigae (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Auriga
Right ascension  05h 40m 42.050s[1]
Declination +31° 55′ 14.20″[1]
Characteristics
Evolutionary stage Asymptotic giant branch[2]
Spectral type M2S Iab[3]
U−B color index +2.22[4]
B−V color index +2.09[4]
R−I color index +1.41[4]
Variable type LC[3]
Astrometry
Radial velocity (Rv)7.21±0.45[5] 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[1] mas
Distanceapprox. 3,500 ly
(approx. 1,100 pc)
Absolute magnitude (MV)−5.88[6]
Details
Mass4.93±1.18[7] M☉
Radius439 ± 61[8] R☉
Luminosity30,900[8] L☉
Surface gravity (log g)−0.037[9] cgs
Temperature3,651±31[8] K
Other designations
BD+31°1049, HD 37536, HIP 26718, HR 1939, SAO 58322
Database references
SIMBADdata

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. It is a 6th magnitude star faintly visible to the naked eye under very good observing conditions.

Variability

A light curve for NO Aurigae plotted from Hipparcos data[10]

In 1969, Olin Jeuck Eggen announced that the star, then called HR 1939, is a variable star.[11] It was given its variable star designation in 1972.[12] 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.[13] The maximum visual magnitude range is 6.05–6.50.[13]

Properties

Most studies of NO Aurigae treat it as a red supergiant member of the Auriga OB1 stellar association at about 1.4 kpc.[14][15] On this basis it would have a luminosity around 67,000 L☉ and a radius around 630 R☉.[6][14]

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.[2] Possible detection of Technetium in the spectrum is a symptom of the third dredge-up which occurs only in late AGB stars.[15]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G.  Gaia EDR3 record for this source at VizieR.
  2. ↑ 2.0 2.1 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. doi:10.1051/0004-6361:200809932. Bibcode: 2008A&A...488..675G. 
  3. ↑ 3.0 3.1 Cite error: Invalid <ref> tag; no text was provided for refs named gcvs
  4. ↑ 4.0 4.1 4.2 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. 
  5. ↑ 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. doi:10.1051/0004-6361:20041272. Bibcode: 2005A&A...430..165F. 
  6. ↑ 6.0 6.1 Cite error: Invalid <ref> tag; no text was provided for refs named levesque
  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. doi:10.1002/asna.200911355. Bibcode: 2010AN....331..349H.  NO Aurigae's database entry at VizieR.
  8. ↑ 8.0 8.1 8.2 Taniguchi, Daisuke; Matsunaga, Noriyuki; Jian, Mingjie; Kobayashi, Naoto; Fukue, Kei; Hamano, Satoshi; Ikeda, Yuji; Kawakita, Hideyo et al. (2021-04-01). "Effective temperatures of red supergiants estimated from line-depth ratios of iron lines in the YJ bands, 0.97-1.32μm". Monthly Notices of the Royal Astronomical Society 502 (3): 4210–4226. doi:10.1093/mnras/staa3855. ISSN 0035-8711. Bibcode: 2021MNRAS.502.4210T. 
  9. ↑ 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. doi:10.1093/mnras/stx1433. Bibcode: 2017MNRAS.471..770M. 
  10. ↑ "Hipparcos Tools Interactive Data Access". ESA. https://www.cosmos.esa.int/web/hipparcos/interactive-data-access. 
  11. ↑ Eggen, O. J. (June 1969). "Light Variations of Small Amplitude in the Red Giants of the Disc Population". Information Bulletin on Variable Stars 355: 1. Bibcode: 1969IBVS..355....1E. https://ibvs.konkoly.hu/pub/ibvs/0301/0355.pdf. Retrieved 30 November 2024. 
  12. ↑ Kukarkin, B. V.; Kholopov, P. N.; Kukarkina, N. P.; Perova, N. B. (September 1972). "58th Name-List of Variable Stars". Information Bulletin on Variable Stars 717: 1–36. Bibcode: 1972IBVS..717....1K. https://ibvs.konkoly.hu/pub/ibvs/0701/0717.pdf. Retrieved 30 November 2024. 
  13. ↑ 13.0 13.1 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. 
  14. ↑ 14.0 14.1 Mauron, N.; Josselin, E. (2011). "The mass-loss rates of red supergiants and the de Jager prescription". Astronomy and Astrophysics 526: A156. doi:10.1051/0004-6361/201013993. Bibcode: 2011A&A...526A.156M. 
  15. ↑ 15.0 15.1 Josselin, E.; Plez, B. (2007). "Atmospheric dynamics and the mass loss process in red supergiant stars". Astronomy and Astrophysics 469 (2): 671. doi:10.1051/0004-6361:20066353. Bibcode: 2007A&A...469..671J. 



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