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 42.05023s[1]
Declination +31° 55′ 14.1920″[1]
Apparent magnitude (V) 6.21[2] (6.06 - 6.44[3])
Characteristics
Spectral type M2Iab[2]
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: 0.13 ± 0.47[1] mas/yr
Dec.: -3.65 ± 0.26[1] mas/yr
Parallax (π)1.68 ± 0.47 mas
Distance1,380[6] pc
Absolute magnitude (MV)−5.88[2]
Details
Mass4.93[7] M
Radius630[2] R
Diameter630[2] D
Luminosity75,000[2] L
Surface gravity (log g)0.1[2] cgs
Temperature3,700[2] 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.)

NO Aurigae is a pulsating variable star in the constellation Auriga.

Variability[edit]

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.[8] The maximum visual magnitude range is 6.05–6.50.[8]

Properties[edit]

Most studies of NO Aurigae treat it as a supergiant member of the Auriga OB1 stellar association at about 1.4 kpc.[6][9] On this basis it has a luminosity around 75,000 L and a radius of 630 D.

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.[10] Possible detection of Technetium in the spectrum is a symptom of the third dredge-up which occurs only in late AGB stars.[9] The revised Hipparcos parallax places it at 420 pc, around the third of the distance of Aur OB1, suggesting about a tenth of the derived luminosity for NO Aur. Calculations using this distance give luminosities of 15,600 L, 7,938 L,[11] or 6,968 L.[7]

References[edit]

  1. 1.0 1.1 1.2 1.3 Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653. arXiv:0708.1752. Bibcode 2007A&A...474..653V. doi:10.1051/0004-6361:20078357.
  2. 2.0 2.1 2.2 2.3 2.4 2.5 2.6 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. arXiv:astro-ph/0504337. Bibcode 2005ApJ...628..973L. doi:10.1086/430901.
  3. 3.0 3.1 Samus, N. N.Expression error: Unrecognized word "etal". (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. 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. arXiv:astro-ph/0409579. Bibcode 2005A&A...430..165F. doi:10.1051/0004-6361:20041272.
  6. 6.0 6.1 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.
  7. 7.0 7.1 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
  8. 8.0 8.1 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.
  9. 9.0 9.1 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.
  10. 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. arXiv:0806.4591. Bibcode 2008A&A...488..675G. doi:10.1051/0004-6361:200809932.
  11. McDonald, I.; Zijlstra, A. A.; Boyer, M. L. (2012). "Fundamental Parameters and Infrared Excesses of Hipparcos Stars". Monthly Notices of the Royal Astronomical Society 427 (1): 343–57. arXiv:1208.2037. Bibcode 2012MNRAS.427..343M. doi:10.1111/j.1365-2966.2012.21873.x.


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