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Pi Cassiopeiae

From Wikipedia, the free encyclopedia
Variable star in the constellation Cassiopeia
Pi Cassiopeiae
Location of π Cassiopeiae (circled)
Observation data
EpochJ2000.0      EquinoxJ2000.0 (ICRS)
ConstellationCassiopeia[1]
Right ascension00h 43m 28.070s[2]
Declination+47° 01′ 28.36″[2]
Apparent magnitude (V)+4.949[3]
Characteristics
Evolutionary stageMain sequence
Spectral typeA5V[4] + A5V[5]
B−Vcolor index+0.171[3]
Variable typeEllipsoidal[6]
Astrometry
Radial velocity (Rv)+12.9±0.8[7] km/s
Proper motion (μ)RA: −24.570mas/yr[2]
Dec.: −36.886mas/yr[2]
Parallax (π)18.6293±0.1142 mas[2]
Distance175 ± 1 ly
(53.7 ± 0.3 pc)
Absolute magnitude (MV)+1.30[1]
Orbit[8]
Period (P)1.9642 d
Eccentricity (e)0.00
Periastronepoch (T)2427535.74 JD
Argument of periastron (ω)
(secondary)
0.00°
Semi-amplitude (K1)
(primary)
120.5 km/s
Semi-amplitude (K2)
(secondary)
122.1 km/s
Details
A
Mass1.82[2] M
Radius1.9[5] R
Luminosity22[9] L
Surface gravity (log g)4.41[10] cgs
Temperature8,392±285[10] K
Rotational velocity (v sin i)60[5] km/s
Age251[10] Myr
B
Mass1.87[2] M
Radius1.9[5] R
Rotational velocity (v sin i)65[5] km/s
Other designations
π Cas,20 Cas,BD+46°146,HD 4058,HIP 3414,HR 184,SAO 36602[11]
Database references
SIMBADdata

Pi Cassiopeiae is a closebinary star[8] system in theconstellationCassiopeia, near the southern border withAndromeda. Its name is aBayer designation that isLatinized from π Cassiopeiae, and abbreviated Pi Cas or π Cas. This system is visible to thenaked eye as a point of light with a combinedapparent visual magnitude of +4.949.[3] Based upon an annualparallax shift of18.63 mas as seen from Earth,[2] this system is located about 175light-years (54 pc) 175 light years from theSun. It is drifting further away with aradial velocity of +13 km/s.[7]

Alight curve for Pi Cassiopeiae, plotted fromTESS data[12]

This is a double-linedspectroscopic binary system with anorbital period of nearly two days in a circular orbit.[8] It is classified as arotating ellipsoidalvariable star and its brightness varies by 0.02 magnitudes with a period of 23.57 hours,[6] which equals half of its orbital period. Thespectrum matches that of anA-type main-sequence star with astellar classification of A5 V.[4] The two stars have similar masses and spectra.[5] A star at a projected separation of1,700 AU has been identified as a possiblewhite dwarf. It is at the same distance as Pi Cassiopeiae and shares acommon proper motion. The age of the white dwarf is calculated to be about 500 million years.[13]

Pi Cassiopeiae has been given the spectral class of kA3hF1mA5, indicating anAm star,[14] but this is now considered doubtful.[15]

References

[edit]
  1. ^abAnderson, 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. XHIP record for this object atVizieR.
  2. ^abcdefgVallenari, A.; et al. (Gaia collaboration) (2023),"Gaia Data Release 3. Summary of the content and survey properties",Astronomy and Astrophysics,674: A1,arXiv:2208.00211,Bibcode:2023A&A...674A...1G,doi:10.1051/0004-6361/202243940,S2CID 244398875. Gaia DR3 record for this source atVizieR.
  3. ^abcHøg, E.; et al. (2000), "The Tycho-2 catalogue of the 2.5 million brightest stars",Astronomy and Astrophysics,355: L27,Bibcode:2000A&A...355L..27H,doi:10.1888/0333750888/2862.
  4. ^abCowley, A.; et al. (April 1969), "A study of the bright A stars. I. A catalogue of spectral classifications",Astronomical Journal,74:375–406,Bibcode:1969AJ.....74..375C,doi:10.1086/110819.
  5. ^abcdefHowe, K. S.; Clarke, C. J. (2009), "An analysis of v sin (I) correlations in early-type binaries",Monthly Notices of the Royal Astronomical Society,392 (1): 448,Bibcode:2009MNRAS.392..448H,doi:10.1111/j.1365-2966.2008.14073.x,S2CID 120183969.
  6. ^abSamus, N. N.; et al. (2017), "General Catalogue of Variable Stars",Astronomy Reports, GCVS 5.1,61 (1):80–88,Bibcode:2017ARep...61...80S,doi:10.1134/S1063772917010085,S2CID 125853869.
  7. ^abde Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project",Astronomy & Astrophysics,546: 14,arXiv:1208.3048,Bibcode:2012A&A...546A..61D,doi:10.1051/0004-6361/201219219,S2CID 59451347, A61.
  8. ^abcPourbaix, D.; et al. (2004), "SB9: The Ninth Catalogue of Spectroscopic Binary Orbits",Astronomy & Astrophysics,424:727–732,arXiv:astro-ph/0406573,Bibcode:2004A&A...424..727P,doi:10.1051/0004-6361:20041213,S2CID 119387088.
  9. ^McDonald, I.; et al. (2012), "Fundamental Parameters and Infrared Excesses of Hipparcos Stars",Monthly Notices of the Royal Astronomical Society,427 (1):343–57,arXiv:1208.2037,Bibcode:2012MNRAS.427..343M,doi:10.1111/j.1365-2966.2012.21873.x,S2CID 118665352.
  10. ^abcDavid, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets",The Astrophysical Journal,804 (2): 146,arXiv:1501.03154,Bibcode:2015ApJ...804..146D,doi:10.1088/0004-637X/804/2/146,S2CID 33401607.
  11. ^"pi. Cas",SIMBAD,Centre de données astronomiques de Strasbourg, retrieved2017-08-30.
  12. ^MAST: Barbara A. Mikulski Archive for Space Telescopes, Space Telescope Science Institute, retrieved8 December 2021.
  13. ^Qiu, Dan; et al. (2021), "Precise Ages of Field Stars from White Dwarf Companions in Gaia DR2",The Astrophysical Journal Supplement Series,253 (2): 58,arXiv:2012.04890,Bibcode:2021ApJS..253...58Q,doi:10.3847/1538-4365/abe468,S2CID 234867350.
  14. ^Abt, Helmut A.; Morrell, Nidia I. (1995), "The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars",Astrophysical Journal Supplement Series,99: 135,Bibcode:1995ApJS...99..135A,doi:10.1086/192182.
  15. ^Renson, P.; Manfroid, J. (2009), "Catalogue of Ap, HGMN and Am stars",Astronomy and Astrophysics,498 (3): 961,Bibcode:2009A&A...498..961R,doi:10.1051/0004-6361/200810788.
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