Misplaced Pages

15 Cancri

Article snapshot taken from[REDACTED] with creative commons attribution-sharealike license. Give it a read and then ask your questions in the chat. We can research this topic together.
Star in the constellation Cancer
15 Cancri

A light curve for BM Cancri, plotted from TESS data
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cancer
Right ascension 08 13 08.87009
Declination +29° 39′ 23.5777″
Apparent magnitude (V) 5.53 - 5.65
Characteristics
Spectral type A0:V:spSiSr
B−V color index −0.073±0.002
Variable type α CVn
Astrometry
Radial velocity (Rv)25.0±0.8 km/s
Proper motion (μ) RA: −12.959 mas/yr
Dec.: −22.232 mas/yr
Parallax (π)3.3279 ± 0.2458 mas
Distance980 ± 70 ly
(300 ± 20 pc)
Absolute magnitude (MV)−0.97
Orbit
Primary15 Cancri A
Companion15 Cancri B
Period (P)635.73±0.53 days
Eccentricity (e)0.55±0.08
Periastron epoch (T)2422045±18
Argument of periastron (ω)
(primary)		196±13°
Semi-amplitude (K1)
(primary)		9.6±1.1 km/s
Details
15 Cnc A
Luminosity327.24 L☉
Surface gravity (log g)3.22±0.2 cgs
Temperature10,080±200 K
Rotational velocity (v sin i)25 km/s
Other designations
15 Cnc, BM Cnc, BD+30°1664, HD 68351, HIP 40240, HR 3215, GSC 01939-01462
Database references
SIMBADdata

15 Cancri is an α CVn-type variable star in the zodiac constellation of Cancer, located around 980 light years away. It has the variable star designation BM Cancri (BM Cnc); 15 Cancri (15 Cnc) is the Flamsteed designation. This system is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of about 5.6. It is moving away from the Earth with a heliocentric radial velocity of 25 km/s.

Radial velocity measurements taken at the Dominion Astrophysical Observatory in Victoria, British Columbia Canada in 1918 and 1919 led to the determination that 15 Cancri is a single-lined spectroscopic binary system. The first orbit was calculated in 1973 by Helmut Abt and Michael Snowden with a period of 585 days however later measurements showed that the orbital period was 635 days.

15 Cancri A, the visible component, is an Ap star, a chemically peculiar star with an over-abundance of iron peak elements, particularly silicon, chromium, and strontium, in its spectrum.

Like all Ap stars, 15 Cancri has a strong magnetic field. This magnetic field varies as it rotates and in 1968 the visual brightness of the star was shown to vary regularly over about four days. 15 Cancri was given the variable star designation BM Cancri in 1972 as a member of the α CVn class of variable stars. The period has since been measured more accurately at 3.3095 d, believed to be the rotational period of the star.

Notes

  1. ^ An alternate period of 475 days is possible but less likely.

References

  1. "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  2. ^ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  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. ^ Abt, Helmut A.; Morrell, Nidia I. (1995). "The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars". Astrophysical Journal Supplement. 99: 135. Bibcode:1995ApJS...99..135A. doi:10.1086/192182.
  5. ^ Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
  6. ^ Stickland, D. J.; Weatherby, J. (1984). "Radial velocities of northern Mercury stars". Astronomy and Astrophysics Supplement Series. 57: 55–67. Bibcode:1984A&AS...57...55S.
  7. ^ Khalack, V.; LeBlanc, F. (2015). "Project VeSElkA: Analysis of Balmer Line Profiles of Slowly Rotating Chemically Peculiar Stars". The Astronomical Journal. 150 (1). 2. arXiv:1505.08158. Bibcode:2015AJ....150....2K. doi:10.1088/0004-6256/150/1/2. S2CID 118283214.
  8. SIMBAD, 15 Cancri (accessed 2012 March 20)
  9. Plaskett, J. S.; et al. (1919). "Fourth list of spectroscopic binaries". Journal of the Royal Astronomical Society of Canada. 13: 372–378. Bibcode:1919JRASC..13..372P.
  10. Abt, Helmut A.; Snowden, Michael S. (1973). "The Binary Frequency for AP Stars". Astrophysical Journal Supplement. 25: 137–162. Bibcode:1973ApJS...25..137A. doi:10.1086/190265.
  11. Renson, P.; Manfroid, J. (2009). "Catalogue of Ap, Hg Mn and Am stars". Astronomy & Astrophysics. 498 (3): 961–966. Bibcode:2009A&A...498..961R. doi:10.1051/0004-6361/200810788.
  12. Stepien, K. (1968). "Photometric behavior of magnetic stars". The Astrophysical Journal. 154: 945. Bibcode:1968ApJ...154..945S. doi:10.1086/149815.
  13. Martins, D. H. (1972). "New Southern Variable Stars". Information Bulletin on Variable Stars. 705: 1. Bibcode:1972IBVS..705....1M.
  14. Wraight, K. T.; Fossati, L.; Netopil, M.; Paunzen, E.; Rode-Paunzen, M.; Bewsher, D.; Norton, A. J.; White, Glenn J. (2012). "A photometric study of chemically peculiar stars with the STEREO satellites - I. Magnetic chemically peculiar stars★". Monthly Notices of the Royal Astronomical Society. 420 (1): 757–772. arXiv:1110.6283. Bibcode:2012MNRAS.420..757W. doi:10.1111/j.1365-2966.2011.20090.x. S2CID 14811051.
Constellation of Cancer
Stars
Bayer
Flamsteed
Variable
HD
Other
Exoplanets
Star clusters
Nebulae
Galaxies
NGC
Other
Galaxy clusters
Category
Categories:
15 Cancri Add topic