15 Arietis

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15 Arietis
15AriLightCurve.png
A visual band light curve for 15 Arietis, plotted from data presented by Tabur et al. (2009) [1]
Observation data
Epoch J2000       Equinox J2000
Constellation Aries
Right ascension 02h 10m 37.59642s [2]
Declination +19° 30′ 01.2099″ [2]
Apparent magnitude  (V)5.67 - 5.74 [3]
Characteristics
Evolutionary stage AGB [4]
Spectral type M3 III [1]
U−B color index +1.91 [5]
B−V color index +1.64 [5]
Variable type SRs [3]
Astrometry
Radial velocity (Rv)+62.04 ± 0.22 [6] km/s
Proper motion (μ)RA: +87.88 [2] mas/yr
Dec.: -27.82 [2] mas/yr
Parallax (π)5.84±0.49  mas [2]
Distance 560 ± 50  ly
(170 ± 10  pc)
Absolute magnitude  (MV)−0.9 [7]
Details
Mass 1.4 [7]   M☉
Radius 87 [7]   R☉
Luminosity 781 [8]   L☉
Temperature 3,565 [8]   K
Other designations
AV  Arietis, BD+18°277, FK5  1056, HD  13325, HIP  10155, HR  631, SAO  92822
Database references
SIMBAD data

15 Arietis (abbreviated 15 Ari) is a single [9] variable star in the northern constellation of Aries. 15 Arietis is the Flamsteed designation; it also bears the variable star designation AV Arietis. It has an apparent visual magnitude of 5.74, [9] which is just bright enough to be visible to the naked eye from dark suburban skies. An annual parallax shift of 5.84  mas [2] corresponds to a physical distance of approximately 560 light-years (170 parsecs ) from Earth. At that distance, the star's brightness is reduced by 0.33 [6] in magnitude because of extinction from interstellar gas and dust.

This is a red giant star with a stellar classification of M3 III. [1] The measured angular diameter of this star is 3.67 ± 0.11 mas. [10] At its estimated distance, [2] this yields a physical size of about 67 times the radius of the Sun. [11] The radius determined from the observed brightness and colour of the star is 87 R☉. [7]

15 Arietis is a short period semiregular variable with the designation AV Arietis. The period given in the General Catalogue of Variable Stars is 5.032 days. [3] Longterm photometry finds that the strongest pulsation period is 18.1 days with an amplitude of 0.028 magnitudes, while a second is 21.9 days and 0.030 in magnitude. [1]

References

  1. 1 2 3 4 Tabur, V.; et al. (December 2009), "Long-term photometry and periods for 261 nearby pulsating M giants", Monthly Notices of the Royal Astronomical Society , 400 (4): 1945–1961, arXiv: 0908.3228 , Bibcode:2009MNRAS.400.1945T, doi: 10.1111/j.1365-2966.2009.15588.x , S2CID   15358380.
  2. 1 2 3 4 5 6 7 van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv: 0708.1752 , Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID   18759600.
  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. ↑ Eggen, Olin J. (1992). "Asymptotic Giant Branch Stars Near the Sun". The Astronomical Journal. 104: 275. Bibcode:1992AJ....104..275E. doi:10.1086/116239.
  5. 1 2 Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. Bibcode:1986EgUBV........0M.
  6. 1 2 Famaey, B.; et al. (January 2005), "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters", Astronomy and Astrophysics, 430 (1): 165–186, arXiv: astro-ph/0409579 , Bibcode:2005A&A...430..165F, doi:10.1051/0004-6361:20041272, S2CID   17804304.
  7. 1 2 3 4 Koen, Chris; Laney, Dave (2000). "Rapidly oscillating M giant stars?". Monthly Notices of the Royal Astronomical Society. 311 (3): 636. Bibcode:2000MNRAS.311..636K. doi: 10.1046/j.1365-8711.2000.03127.x .
  8. 1 2 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): 343–357. arXiv: 1208.2037 . Bibcode:2012MNRAS.427..343M. doi: 10.1111/j.1365-2966.2012.21873.x . S2CID   118665352.
  9. 1 2 Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv: 0806.2878 , Bibcode:2008MNRAS.389..869E, doi: 10.1111/j.1365-2966.2008.13596.x , S2CID   14878976.
  10. ↑ Richichi, A.; Percheron, I.; Khristoforova, M. (February 2005), "CHARM2: An updated Catalog of High Angular Resolution Measurements", Astronomy and Astrophysics, 431 (2): 773–777, Bibcode:2005A&A...431..773R, doi: 10.1051/0004-6361:20042039 .
  11. ↑ Lang, Kenneth R. (2006), Astrophysical formulae, Astronomy and astrophysics library, vol. 1 (3rd ed.), Birkhäuser, ISBN   3-540-29692-1.. The radius (R*) is given by:
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