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Pi Cassiopeiae

January 07, 2023

Pi Cassiopeiae, Latinized from π Cassiopeiae, is a close binary star[8] system in the constellation Cassiopeia. It is visible to the naked eye with an apparent visual magnitude of +4.949.[2] Based upon an annual parallax shift of 18.63 mas as seen from Earth,[1] this system is located about 175 light years from the Sun.

Pi Cassiopeiae

Map of the Bayer-designated stars in Cassiopeia. Pi Cassiopeiae is circled.
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Cassiopeia
Right ascension 00h 43m 28.07045s[1]
Declination +47° 01′ 28.3694″[1]
Apparent magnitude (V) +4.949[2]
Characteristics
Spectral type A5V[3] + A5V[4]
B−V color index +0.171[2]
Variable type Ellipsoidal[5]
Astrometry
Radial velocity (Rv)+12.9±0.8[6] km/s
Proper motion (μ) RA: −23.71±0.23[1] mas/yr
Dec.: −36.84±0.18[1] mas/yr
Parallax (π)18.63 ± 0.32 mas[1]
Distance175 ± 3 ly
(53.7 ± 0.9 pc)
Absolute magnitude (MV)+1.30[7]
Orbit[8]
Period (P)1.9642 d
Eccentricity (e)0.00
Periastron epoch (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[9] M☉
Radius1.9[4] R☉
Luminosity22[10] L☉
Surface gravity (log g)4.41[11] cgs
Temperature8,392±285[11] K
Rotational velocity (v sin i)60[4] km/s
Age251[11] Myr
B
Mass1.87[9] M☉
Radius1.9[4] R☉
Rotational velocity (v sin i)65[4] km/s
Other designations
π Cas, 20 Cas, BD+46°146, HD 4058, HIP 3414, HR 184, SAO 36602[12]
Database references
SIMBADdata
A light curve for Pi Cassiopeiae, plotted from TESS data[13]

This is a double-lined spectroscopic binary system with an orbital period of nearly two days in a circular orbit.[8] It is classified as a rotating ellipsoidal variable star and its brightness varies by 0.02 magnitudes with a period of 23.57 hours,[5] which equals half of its orbital period. The spectrum matches that of an A-type main-sequence star with a stellar classification of A5 V.[3] The two stars have similar masses and spectra.[4] A star at a projected separation of 1,700 AU has been identified as a possible white dwarf. It is at the same distance as Pi Cassiopeiae and shares a common proper motion. The age of the white dwarf is calculated to be about 500 million years.[14]

Pi Cassiopeiae has been given the spectral class of kA3hF1mA5, indicating an Am star,[15] but this is now considered doubtful.[16]

References

  1. ^ a b c d e f van Leeuwen, F. (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.
  2. ^ a b c Høg, 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.
  3. ^ a b Cowley, 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.
  4. ^ a b c d e f Howe, 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.
  5. ^ a b Samus, 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.
  6. ^ de 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.
  7. ^ 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.
  8. ^ a b c Pourbaix, 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. ^ a b Vallenari, A.; et al. (Gaia Collaboration) (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. arXiv:2208.00211. doi:10.1051/0004-6361/202243940. Gaia DR3 record for this source at VizieR.
  10. ^ 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.
  11. ^ a b c David, 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.
  12. ^ "pi. Cas". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-08-30.
  13. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  14. ^ Qiu, Dan; Tian, Hai-Jun; Wang, Xi-Dong; Nie, Jia-Lu; von Hippel, Ted; Liu, Gao-Chao; Fouesneau, Morgan; Rix, Hans-Walter (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.
  15. ^ 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.
  16. ^ 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.

January 07, 2023
cassiopeiae, latinized, from, cassiopeiae, close, binary, star, system, constellation, cassiopeia, visible, naked, with, apparent, visual, magnitude, based, upon, annual, parallax, shift, seen, from, earth, this, system, located, about, light, years, from, bay. Pi Cassiopeiae Latinized from p Cassiopeiae is a close binary star 8 system in the constellation Cassiopeia It is visible to the naked eye with an apparent visual magnitude of 4 949 2 Based upon an annual parallax shift of 18 63 mas as seen from Earth 1 this system is located about 175 light years from the Sun Pi CassiopeiaeMap of the Bayer designated stars in Cassiopeia Pi Cassiopeiae is circled Observation dataEpoch J2000 0 Equinox J2000 0 ICRS Constellation CassiopeiaRight ascension 00h 43m 28 07045s 1 Declination 47 01 28 3694 1 Apparent magnitude V 4 949 2 CharacteristicsSpectral type A5V 3 A5V 4 B V color index 0 171 2 Variable type Ellipsoidal 5 AstrometryRadial velocity Rv 12 9 0 8 6 km sProper motion m RA 23 71 0 23 1 mas yr Dec 36 84 0 18 1 mas yrParallax p 18 63 0 32 mas 1 Distance175 3 ly 53 7 0 9 pc Absolute magnitude MV 1 30 7 Orbit 8 Period P 1 9642 dEccentricity e 0 00Periastron epoch T 2427535 74 JDArgument of periastron w secondary 0 00 Semi amplitude K1 primary 120 5 km sSemi amplitude K2 secondary 122 1 km sDetailsAMass1 82 9 M Radius1 9 4 R Luminosity22 10 L Surface gravity log g 4 41 11 cgsTemperature8 392 285 11 KRotational velocity v sin i 60 4 km sAge251 11 MyrBMass1 87 9 M Radius1 9 4 R Rotational velocity v sin i 65 4 km sOther designationsp Cas 20 Cas BD 46 146 HD 4058 HIP 3414 HR 184 SAO 36602 12 Database referencesSIMBADdata A light curve for Pi Cassiopeiae plotted from TESS data 13 This is a double lined spectroscopic binary system with an orbital period of nearly two days in a circular orbit 8 It is classified as a rotating ellipsoidal variable star and its brightness varies by 0 02 magnitudes with a period of 23 57 hours 5 which equals half of its orbital period The spectrum matches that of an A type main sequence star with a stellar classification of A5 V 3 The two stars have similar masses and spectra 4 A star at a projected separation of 1 700 AU has been identified as a possible white dwarf It is at the same distance as Pi Cassiopeiae and shares a common proper motion The age of the white dwarf is calculated to be about 500 million years 14 Pi Cassiopeiae has been given the spectral class of kA3hF1mA5 indicating an Am star 15 but this is now considered doubtful 16 References Edit a b c d e f van Leeuwen F 2007 Validation of the new Hipparcos reduction Astronomy and Astrophysics 474 2 653 664 arXiv 0708 1752 Bibcode 2007A amp A 474 653V doi 10 1051 0004 6361 20078357 S2CID 18759600 a b c Hog E et al 2000 The Tycho 2 catalogue of the 2 5 million brightest stars Astronomy and Astrophysics 355 L27 Bibcode 2000A amp A 355L 27H doi 10 1888 0333750888 2862 a b Cowley 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 a b c d e f Howe 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 a b Samus 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 de Bruijne J H J Eilers A C October 2012 Radial velocities for the HIPPARCOS Gaia Hundred Thousand Proper Motion project Astronomy amp Astrophysics 546 14 arXiv 1208 3048 Bibcode 2012A amp A 546A 61D doi 10 1051 0004 6361 201219219 S2CID 59451347 A61 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 a b c Pourbaix D et al 2004 SB9 The Ninth Catalogue of Spectroscopic Binary Orbits Astronomy amp Astrophysics 424 727 732 arXiv astro ph 0406573 Bibcode 2004A amp A 424 727P doi 10 1051 0004 6361 20041213 S2CID 119387088 a b Vallenari A et al Gaia Collaboration 2022 Gaia Data Release 3 Summary of the content and survey properties Astronomy amp Astrophysics arXiv 2208 00211 doi 10 1051 0004 6361 202243940 Gaia DR3 record for this source at VizieR 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 a b c David Trevor J Hillenbrand Lynne A 2015 The Ages of Early Type Stars Stromgren 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 pi Cas SIMBAD Centre de donnees astronomiques de Strasbourg Retrieved 2017 08 30 MAST Barbara A Mikulski Archive for Space Telescopes Space Telescope Science Institute Retrieved 8 December 2021 Qiu Dan Tian Hai Jun Wang Xi Dong Nie Jia Lu von Hippel Ted Liu Gao Chao Fouesneau Morgan Rix Hans Walter 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 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 Renson P Manfroid J 2009 Catalogue of Ap HGMN and Am stars Astronomy and Astrophysics 498 3 961 Bibcode 2009A amp A 498 961R doi 10 1051 0004 6361 200810788 Retrieved from https en wikipedia org w index php title Pi Cassiopeiae amp oldid 1126508424, wikipedia, wiki, book, books, library,

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