15 Arietis

Today, 15 Arietis is a topic of great relevance in society. Since its emergence, it has captured the attention of people of all ages and interests. Whether due to its impact on popular culture, its influence in the scientific field or its importance in everyday life, 15 Arietis has become a topic that does not go unnoticed. Over the years, it has generated debates, research and advances that have transformed the way we understand the world around us. In this article, we will explore different aspects related to 15 Arietis, its evolution over time, its importance today, and its possible influence in the future.

15 Arietis

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
Spectral type M3 III[1]
U−B color index +1.91[4]
B−V color index +1.64[4]
Variable type SRs[3]
Astrometry
Radial velocity (Rv)+62.04 ± 0.22[5] 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]
Distance560 ± 50 ly
(170 ± 10 pc)
Absolute magnitude (MV)−0.9[6]
Details
Mass1.4[6] M☉
Radius87[6] R☉
Luminosity781[7] L☉
Temperature3,565[7] K
Other designations
AV Arietis, BD+18°277, FK5 1056, HD 13325, HIP 10155, HR 631, SAO 92822
Database references
SIMBADdata

15 Arietis (abbreviated 15 Ari) is a single[8] 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,[8] 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[5] 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.[9] At its estimated distance,[2] this yields a physical size of about 67 times the radius of the Sun.[10] The radius determined from the observed brightness and colour of the star is 87 R☉.[6]

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. ^ a b c d 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. ^ a b c d e f g 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. ^ a b c 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. ^ a b Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. Bibcode:1986EgUBV........0M.
  5. ^ a b 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.
  6. ^ a b c d 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.
  7. ^ a b 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.
  8. ^ a b 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.
  9. ^ 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.
  10. ^ 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: