Astronomy:59 Aurigae

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Short description: Star in the constellation Auriga
59 Aurigae
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Four visual band light curves for 59 Aurigae, adapted from Zhiping (2000)[1]
Observation data
Equinox J2000.0]] (ICRS)
Constellation Auriga
Right ascension  06h 53m 01.41097s[2]
Declination +38° 52′ 08.9322″[2]
Apparent magnitude (V) 6.099[3]
Characteristics
Evolutionary stage subgiant[2]
Spectral type F2V[4]
U−B color index +0.14[5]
B−V color index +0.38[5]
Variable type δ Sct[6]
Astrometry
Radial velocity (Rv)1.0±4.3[7] km/s
Proper motion (μ) RA: −3.916[2] mas/yr
Dec.: +6.659[2] mas/yr
Parallax (π)6.7702 ± 0.0476[2] mas
Distance482 ± 3 ly
(148 ± 1 pc)
Absolute magnitude (MV)0.23±0.12[8]
Details
Mass2.37[9] M☉
Radius5.7[10] R☉
Luminosity62[2] L☉
Surface gravity (log g)3.23[9] cgs
Temperature6,848[10] K
Metallicity [Fe/H]0.18[8] dex
Rotational velocity (v sin i)165[11] km/s
Age530[12] Myr
Other designations
59 Aur, OX Aur, BD+39°1771, GC 8993, HD 50018, HIP 33041, HR 2539, SAO 59571, PPM 72197, ADS 5534, CCDM J06530+3852, WDS J06530+3852, TYC 2942-2005-1, GSC 02942-02005
Database references
SIMBADdata

59 Aurigae, often abbreviated as 59 Aur, is a star in the constellation Auriga. Its baseline apparent magnitude is 6.1,[3] meaning it can just barely be seen with the naked eye as a dim, yellow-white hued star. Based on parallax measurements, it is located about 482 light-years (148 parsecs) away from the Sun.[2]

In 1966, Ivan John Danziger and Robert John Dickens discovered that 59 Aurigae star is a variable star.[13] This object is a Delta Scuti variable, meaning it varies in luminosity due to pulsations on its surface, ranging in magnitude from 5.94 down to 6.14 with a period of 0.154412 days (3.7 h).[6] For that reason, in 1975, it was given the variable star designation OX Aurigae.[14] The star's spectrum matches that of an F-type main-sequence star and it has a spectral type of F2V.[4] It has 2.4 times the mass of the Sun[9] and 5.7 times the Sun's radius.[10] 59 Aurigae is thought to be around 530 million years old,[12] and is radiating 62 times the Sun's luminosity[2] from its photosphere an effective temperature of 6,848 K.[10]

References

  1. ↑ Zhiping, Li (October 2000). "Complicated pulsation in the delta Scuti variable 59 Aurigae". Astronomy and Astrophysics 362: 595–598. Bibcode: 2000A&A...362..595L. https://ui.adsabs.harvard.edu/abs/2000A&A...362..595L. Retrieved 31 October 2021. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 2.7 2.8 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.
  3. ↑ 3.0 3.1 Høg, E. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics 355: L27–L30. Bibcode: 2000A&A...355L..27H. 
  4. ↑ 4.0 4.1 Abt, Helmut A.; Morrell, Nidia I. (1995). "The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars". Astrophysical Journal Supplement 99: 135. doi:10.1086/192182. Bibcode: 1995ApJS...99..135A. 
  5. ↑ 5.0 5.1 Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. Bibcode: 1986EgUBV........0M. 
  6. ↑ 6.0 6.1 Samus, N. N. et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1 61 (1): 80–88, doi:10.1134/S1063772917010085, Bibcode: 2017ARep...61...80S. 
  7. ↑ Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters 32 (11): 759–771. doi:10.1134/S1063773706110065. Bibcode: 2006AstL...32..759G. 
  8. ↑ 8.0 8.1 Nordström, B. (2004). "The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ˜14 000 F and G dwarfs". Astronomy and Astrophysics 418: 989–1019. doi:10.1051/0004-6361:20035959. Bibcode: 2004A&A...418..989N. 
  9. ↑ 9.0 9.1 9.2 Anders, F.; Khalatyan, A.; Queiroz, A. B. A.; Chiappini, C.; Ardèvol, J.; Casamiquela, L.; Figueras, F.; Jiménez-Arranz, Ó. et al. (2022). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia EDR3 stars brighter than G = 18.5". Astronomy and Astrophysics 658: A91. doi:10.1051/0004-6361/202142369. Bibcode: 2022A&A...658A..91A. 
  10. ↑ 10.0 10.1 10.2 10.3 Fetherolf, Tara; Pepper, Joshua; Simpson, Emilie; Kane, Stephen R.; Močnik, Teo; English, John Edward; Antoci, Victoria; Huber, Daniel et al. (2023). "Variability Catalog of Stars Observed during the TESS Prime Mission". The Astrophysical Journal Supplement Series 268 (1): 4. doi:10.3847/1538-4365/acdee5. Bibcode: 2023ApJS..268....4F. 
  11. ↑ Zorec, J.; Royer, F. (2012). "Rotational velocities of A-type stars. IV. Evolution of rotational velocities". Astronomy & Astrophysics 537: A120. doi:10.1051/0004-6361/201117691. A120. Bibcode: 2012A&A...537A.120Z. 
  12. ↑ 12.0 12.1 Pace, G. (2013). "Chromospheric activity as age indicator. An L-shaped chromospheric-activity versus age diagram". Astronomy and Astrophysics 551. doi:10.1051/0004-6361/201220364. Bibcode: 2013A&A...551L...8P. 
  13. ↑ Danziger, I. J.; Dickens, R. J. (August 1966). "Observations of Variable F-Type Stars with Short Periods". Information Bulletin on Variable Stars 150. Bibcode: 1966IBVS..150....1D. https://ibvs.konkoly.hu/pub/ibvs/0101/0150.pdf. Retrieved 29 November 2024. 
  14. ↑ Kukarkin, B. V.; Kholopov, P. N.; Kukarkina, N. P. (November 1975). "61st Name-List of Variable Stars". Information Bulletin on Variable Stars 1068: 1–5. Bibcode: 1975IBVS.1068....1K. https://ibvs.konkoly.hu/pub/ibvs/1001/1068.pdf. Retrieved 30 November 2024. 



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