15 Arietis

Last updated
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
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]
Distance 560 ± 50  ly
(170 ± 10  pc)
Absolute magnitude  (MV)−0.9 [6]
Details
Mass 1.4 [6]   M☉
Radius 87 [6]   R☉
Luminosity 781 [7]   L☉
Temperature 3,565 [7]   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 [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 the estimated distance of Delta Ophiuchi, [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]

Related Research Articles

<span class="mw-page-title-main">Iota Sagittarii</span> Astrometric binary star in the constellation Sagittarius

Iota Sagittarii is a star in the zodiac constellation of Sagittarius. With an apparent visual magnitude of +4.118, it is bright enough to be viewed with the naked eye. Based upon an annual parallax shift of 17.94 mas as seen from Earth, this star is located 182 light years from the Sun. It is moving away from the Earth with a radial velocity of +35.8 km/s.

Pi Tauri is a solitary, yellow-hued star in the zodiac constellation of Taurus. With an apparent visual magnitude of +4.69, it is bright enough to be visible to the naked eye. Although it appears to lie among the stars of the Hyades cluster, it is not itself a member, being three times farther from Earth than the cluster. The distance to this star, as determined using an annual parallax shift of 7.83 mas as seen from the Earth, is around 420 light years. At that range, the visual magnitude of the star is diminished by an extinction factor of 0.24 due to interstellar dust.

<span class="mw-page-title-main">Rho Ursae Majoris</span> Solitary red giant star in the constellation Ursa Major

Rho Ursae Majoris (ρ UMa) is the Bayer designation for a solitary star in the northern circumpolar constellation of Ursa Major. It is faintly visible to the naked eye with an apparent visual magnitude of 4.74. The distance to this star, based upon an annual parallax shift of 10.37 mas, is around 315 light years.

<span class="mw-page-title-main">Chi Aquarii</span> Star in the constellation Aquarius

Chi Aquarii, Latinized from χ Aquarii, is the Bayer designation of a star in the equatorial constellation of Aquarius. The distance to this star, based upon parallax measurements with a 7% margin of error, is roughly 610 light-years. It is visible to the naked eye with an apparent visual magnitude of about 5.

<span class="mw-page-title-main">3 Aquarii</span> Star in the constellation Aquarius

3 Aquarii is a variable star in the equatorial constellation of Aquarius. 3 Aquarii is the Flamsteed designation; it also bears the Bayer designation k Aquarii and the variable star designation EN Aquarii. With a mean apparent visual magnitude of 4.429, it is visible to the naked eye in dark skies. It has an annual parallax shift of 5.57 milliarcseconds with a 5% margin of error, which translates to a physical distance of around 590 light-years from Earth.

<span class="mw-page-title-main">2 Centauri</span> Star in the constellation Centaurus

2 Centauri is a single star in the southern constellation of Centaurus, located approximately 183 light-years from Earth. It has the Bayer designation g Centauri; 2 Centauri is the Flamsteed designation. This object is visible to the naked eye as faint, red-hued star with an apparent visual magnitude of 4.19. It is moving away from the Earth with a heliocentric radial velocity of +41 km/s. The star is a member of the HR 1614 supercluster.

Tau<sup>4</sup> Eridani Binary star system in the constellation Eridanus

Tau4 Eridani is a binary star system in the constellation Eridanus. It is visible to the naked eye with an apparent visual magnitude of 3.65. The distance to this star can be estimated using the parallax method, which yields a value of roughly 300 light years.

Theta Geminorum is a single star in the northern zodiac constellation of Gemini. It is visual to the naked eye with an apparent visual magnitude of 3.59. Based upon an annual parallax shift of 17.25 mas, it is about 189 light years distant from the Sun.

Upsilon Librae is the Bayer designation for a double star in the zodiac constellation Libra. With an apparent visual magnitude of 3.628, it is visible to the naked eye. The distance to this star, based upon an annual parallax shift of 14.58, is around 224 light years. It has a magnitude 10.8 companion at an angular separation of 2.0 arc seconds along a position angle of 151°, as of 2002.

Sigma<sup>1</sup> Ursae Majoris Solitary star in the constellation Ursa Major

Sigma1 Ursae Majoris (σ1 UMa) is the Bayer designation for a solitary star in the northern circumpolar constellation of Ursa Major. With an apparent visual magnitude of 5.14 it is faintly visible to the naked eye on dark nights. Based upon an annual parallax shift of 6.26 mas, it is located roughly 520 light years from the Sun. At that distance, the visual magnitude of the star is diminished by an extinction factor of 0.06 due to interstellar dust.

<span class="mw-page-title-main">Nu Orionis</span> Binary star system in the constellation Orion

Nu Orionis is a binary star system in the northeastern part of the constellation Orion. It should not be confused with the variable star NU Orionis. Nu Orionis has an apparent visual magnitude of 4.42, which is bright enough to be seen with the naked eye. Based upon an annual parallax shift of 0.00632 arcseconds, the distance to this system is roughly 520 light years.

Gamma Chamaeleontis, Latinized from γ Chamaeleontis, is a solitary star located in the southern circumpolar constellation of Chamaeleon. It can faintly be seen with the naked eye on a dark night, having an apparent visual magnitude of 4.12. Based upon an annual parallax shift of 7.81 mas, it is located around 418 light years from the Sun.

<span class="mw-page-title-main">47 Cygni</span> Star in the constellation Cygnus

47 Cygni is a triple star system in the northern constellation of Cygnus, and is located around 4,000 light years from the Earth. It is visible to the naked eye with a combined apparent visual magnitude of 4.61. The system is moving closer to the Earth with a heliocentric radial velocity of −4.6 km/s.

φ Eridani is a star in the constellation Eridanus. It is visible to the naked eye with an apparent visual magnitude of 3.55. The distance to this star, as determined using the parallax method, is around 154 light-years.

Pi Eridani, Latinized from π Eridani, is a star in the constellation Eridanus. It has an apparent visual magnitude of 4.40, which is bright enough to be seen on a dark, clear night. Based upon parallax measurements, it is located roughly 480 light years from the Sun.

<span class="mw-page-title-main">Omicron Geminorum</span> Star in the constellation Gemini

Omicron Geminorum, also named Jishui, is a solitary star in the constellation of Gemini. It is faintly visible to the naked eye with an apparent visual magnitude of 4.90. Based upon an annual parallax shift of 19.61 mas, it is located at a distance of 166 light-years from the Sun.

61 Leonis is a possible binary star system in the zodiac constellation of Leo. It is faintly visible to the naked eye, having an apparent visual magnitude of 4.73. The star is moving closer to the Sun with a heliocentric radial velocity of −12.7 km/s. It is located roughly 580 light-years from the Sun, as determined from its annual parallax shift of 5.58 mas.

<span class="mw-page-title-main">GZ Velorum</span> Star in the constellation Vela

GZ Velorum is a single, orange-hued star in the southern constellation of Vela. It is a faint star but visible to the naked eye, having an apparent visual magnitude of 4.58. The star is located around 1,300 light years from Earth, as determined from its annual parallax shift of 2.4 mas. It is moving further away with a heliocentric radial velocity of +13 km/s.

π Geminorum is a star located in the constellation Gemini, to the north of Castor. With an apparent visual magnitude of 5.14, it is faintly visible to the naked eye on a dark night. Based upon an annual parallax|shift of 4.93 mas, Pi Geminorum is located roughly 660 light years from the Sun. At that distance, the visual magnitude of the star is diminished by an interstellar absorption factor of 0.033 due to interstellar dust.

<span class="mw-page-title-main">Omega Geminorum</span> Star in the constellation Gemini

Omega Geminorum, Latinized from ω Geminorum, is a star located in the middle of the northern zodiac constellation of Gemini. With an apparent visual magnitude of 5.18, it is faintly visible to the naked eye. According to the Bortle scale, it can be viewed from dark suburban skies. With an annual parallax shift of just 2.19 mas, it is located about 1,500 light years from the Sun.

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. 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.
  5. 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.
  6. 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 .
  7. 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.
  8. 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.
  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:
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.