Astronomy:Psi1 Aurigae

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Short description: Star in the constellation Auriga
For other stars with this Bayer designation, see ψ Aurigae.
Psi1 Aurigae
Location of ψ1 Aurigae (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Auriga
Right ascension  06h 24m 53.90155s[1]
Declination +49° 17′ 16.4112″[1]
Apparent magnitude (V) 4.91[2]
Characteristics
Evolutionary stage Red supergiant
Spectral type K5-M1Iab-Ib[3]
U−B color index +2.29[2]
B−V color index +1.97[2]
R−I color index 1.07[citation needed]
Variable type LC[4]
Astrometry
Radial velocity (Rv)+4.7[5] km/s
Proper motion (μ) RA: −0.155[1][1] mas/yr
Dec.: −2.131[1] mas/yr
Parallax (π)0.4426 ± 0.1103[1] mas
Distance6,590+1,382
−1,174 ly
(2,021.5+424
−360 pc)
Absolute magnitude (MV)−5.53[6]
Details
Mass14.4±0.8[7] M☉
Radius934 R☉[8]
1,004[9][lower-alpha 1] R☉
Luminosity170,400[8] L☉
Temperature3,790[8] K
Metallicity [Fe/H]+0.08[10] dex
Age12.3±0.4[7] Myr
Other designations
ψ1 Aurigae, 46 Aurigae, BD+49 1488, FK5 242, GC 8235, HD 44537, HIP 30520, HR 2289, SAO 41076, PPM 49029[11]
Database references
SIMBADdata

Psi1 Aurigae is a star in the northern constellation of Auriga. It name is a Bayer designation that is Latinized from ψ1 Aurigae, and abbreviated Psi1 Aur or ψ1 Aur. This star is faintly visible to the naked eye with an apparent visual magnitude of 4.91.[2] Based upon a measured annual parallax shift of 0.44 mas,[1] it is approximately 7,500 light-years (2,300 parsecs) distant from the Earth. It is receding from the Sun with a radial velocity of +4.7 km/s.[5]

Description

A visual band light curve for Psi1 Aurigae, adapted from Percy et al. (2001)[12]

This is a massive supergiant star with a stellar classification of K5-M1Iab-Ib.[3] It is a slow irregular variable of the LC type, with its brightness varying in magnitude by 0.44.[4] The star is more than 14[7] times as massive as the Sun, over 900 times larger, and is blazing with 170,000 times the Sun's luminosity.[8] It is one of the largest stars known, even larger and more luminous than well-known red supergiants Betelgeuse and Antares. This energy is being radiated into outer space from its outer atmosphere at an effective temperature of 3,790 K,[8] giving it the orange-red hue of a cool M-type star.

See also

Notes

  1. ↑ Applying the Stefan–Boltzmann law with a nominal solar effective temperature of 5,772 K:
    (5,7723,740)4⋅105.25=1,004.41 R⊙.

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940.  Gaia DR3 record for this source at VizieR.
  2. ↑ 2.0 2.1 2.2 2.3 Nicolet, B. (1978), "Photoelectric photometric Catalogue of homogeneous measurements in the UBV System", Astronomy and Astrophysics Supplement Series 34: 1–49, Bibcode: 1978A&AS...34....1N. 
  3. ↑ 3.0 3.1 Keenan, Philip C.; McNeil, Raymond C. (1989), "The Perkins Catalog of Revised MK Types for the Cooler Stars", The Astrophysical Journal Supplement Series 71: 245, doi:10.1086/191373, Bibcode: 1989ApJS...71..245K. 
  4. ↑ 4.0 4.1 Adelman, Saul J. (2001), "Stars with the Largest Hipparcos Photometric Amplitudes", Baltic Astronomy 10 (4): 589–593, doi:10.1515/astro-2001-0403, Bibcode: 2001BaltA..10..589A. 
  5. ↑ 5.0 5.1 Wielen, R. et al. (1999), "Sixth Catalogue of Fundamental Stars (FK6). Part I. Basic fundamental stars with direct solutions", Veroeffentlichungen des Astronomischen Rechen-Instituts Heidelberg (Astronomisches Rechen-Institut Heidelberg) 35 (35): 1, Bibcode: 1999VeARI..35....1W. 
  6. ↑ Schiavon, Ricardo P. (July 2007), "Population Synthesis in the Blue. IV. Accurate Model Predictions for Lick Indices and UBV Colors in Single Stellar Populations", The Astrophysical Journal Supplement Series 171 (1): 146–205, doi:10.1086/511753, Bibcode: 2007ApJS..171..146S. 
  7. ↑ 7.0 7.1 7.2 Tetzlaff, N. et al. (January 2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun", Monthly Notices of the Royal Astronomical Society 410 (1): 190–200, doi:10.1111/j.1365-2966.2010.17434.x, Bibcode: 2011MNRAS.410..190T. 
  8. ↑ 8.0 8.1 8.2 8.3 8.4 Healy, Sarah et al. (March 23, 2024), "Red Supergiant Candidates for Multimessenger Monitoring of the Next Galactic Supernova", Monthly Notices of the Royal Astronomical Society 529 (4): 3630–3650, doi:10.1093/mnras/stae738, ISSN 0035-8711, Bibcode: 2024MNRAS.529.3630H. 
  9. ↑ Taniguchi, Daisuke et al. (April 2021), "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. 
  10. ↑ Bakos, Gustav A. (October 1971), "Abundances of Heavy Elements in Late-Type Stars", Journal of the Royal Astronomical Society of Canada 65: 222, Bibcode: 1971JRASC..65..222B. 
  11. ↑ "psi01 Aur". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=psi01+Aur. 
  12. ↑ Percy, John R. et al. (August 2001), "Long-Term VRI Photometry of Small-Amplitude Red Variables. I. Light Curves and Periods", Publications of the Astronomical Society of the Pacific 113 (786): 983–996, doi:10.1086/322153, Bibcode: 2001PASP..113..983P. 
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