Astronomy:HD 4222

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Short description: Binary star; Cassiopeia
HD 4222
Cassiopeia constellation map.svg
Red circle.svg
Location of HD 4222 on the map (circled)
Observation data
{{#ifeq:J2000.0 (ICRS)|J2000.0 (ICRS)|Epoch J2000.0      Equinox J2000.0 (ICRS)| [[History:Epoch|Epoch J2000.0 (ICRS)]]      [[Astronomy:Equinox (celestial coordinates)|Equinox J2000.0 (ICRS)}}
Constellation Cassiopeia
A
Right ascension  00h 45m 17.17365s[1]
Declination +55° 13′ 17.0310″[1]
Apparent magnitude (V) 5.41±0.01[2]
B
Right ascension  00h 45m 17.14092s[3]
Declination +55° 13′ 15.4000″[3]
Apparent magnitude (V) 11.5[4]
Characteristics
A
Evolutionary stage main sequence star[5]
Spectral type A2 Vs[6] or A1 V[7]
U−B color index +0.05[8]
B−V color index +0.04[8]
B
Spectral type M2-5V[9]
Astrometry
Radial velocity (Rv)−8.5±2[10] km/s
Proper motion (μ) RA: −29.935[1] mas/yr
Dec.: −5.616[1] mas/yr
Parallax (π)9.2342 ± 0.0586[1] mas
Distance353 ± 2 ly
(108.3 ± 0.7 pc)
Absolute magnitude (MV)+0.44[11]
Details
A
Mass2.59±0.04[5] M☉
Radius3.47±0.18[12] R☉
Luminosity69.1+5.6−5.2[5] L☉
Surface gravity (log g)3.72+0.08−0.06[13] cgs
Temperature9,886[14] K
Metallicity [Fe/H]−0.26[15] dex
Rotational velocity (v sin i)25±8[7] km/s
Age407+51−52[1] Myr
Other designations
BD+54°143, GC 894, HD 4222, HIP 3544, HR 196, SAO 21677, ADS 625 A, CCDM J00453+5514A, WDS J00453+5513A[16]
Database references
SIMBADdata

HD 4222, also known as HR 196, is the primary of a binary star[17] located in the northern constellation Cassiopeia. It is faintly visible to the naked eye as a white-hued point of light with an apparent magnitude of 5.41.[2] Gaia DR3 parallax measurements imply a distance of 353 light-years and it is drifting closer with a heliocentric radial velocity of −8.5 km/s.[10] At its current distance, HD 4222's brightness is diminished by an interstellar extinction of 0.13 magnitudes and it has an absolute magnitude of +0.44.[11]

HD 4222 has a stellar classification of A2 Vs or A1 V,[6][7] both classes indicating that it is an A-type main-sequence star that is generating energy via hydrogen fusion at its core. The former class includes the presence of 'sharp' or narrow absorption lines due to slow rotation. Consistent with the class, HD 4222 spins modestly with a projected rotational velocity of approximately 25 km/s.[7] It has 2.59 times the mass of the Sun[5] and 3.47 times the radius of the Sun.[12] It radiates 69.1 times the luminosity of the Sun[5] from its photosphere with an effective temperature of 9,886 K.[14] HD 4222 is metal deficient with an iron abundance of [Fe/H] = −0.26 or 55% of the Sun's.[15] At the age of 407 million years,[1] HD 4222 has completed 81.5% of its main sequence lifetime.[5]

HD 4222 and BU 492B make up the binary system BU 492. The companion is a red dwarf with a stellar classification of M2-5V; it is located 1.5" away from the primary along a position angle of 173°. BU 492B was first noticed by astronomer S. W. Burnham in 1878. HD 4222 also has one optical companion; an 11th magnitude star located 88.6" away, which itself is also a double star.[4] A X-ray emission with a luminosity of 3.031×1020 W was detected around the star.[9] A-type stars are not expected to emit X-rays, so it might be coming from the companion. HD 4222 is considered to be a probable member of the Sirius supercluster, a group of stars moving with the bright star Sirius and share a common origin with the system.[18]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  2. ↑ 2.0 2.1 Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P. et al. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics 355: L27–L30. ISSN 0004-6361. Bibcode: 2000A&A...355L..27H. 
  3. ↑ 3.0 3.1 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  4. ↑ 4.0 4.1 Mason, Brian D.; Wycoff, Gary L.; Hartkopf, William I.; Douglass, Geoffrey G.; Worley, Charles E. (December 2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal 122 (6): 3466–3471. doi:10.1086/323920. ISSN 0004-6256. Bibcode: 2001AJ....122.3466M. 
  5. ↑ 5.0 5.1 5.2 5.3 5.4 5.5 Zorec, J.; Royer, F. (January 2012). "Rotational velocities of A-type stars IV: Evolution of rotational velocities". Astronomy & Astrophysics 537: A120. doi:10.1051/0004-6361/201117691. ISSN 0004-6361. Bibcode: 2012A&A...537A.120Z. 
  6. ↑ 6.0 6.1 Cowley, A.; Cowley, C.; Jaschek, M.; Jaschek, C. (April 1969). "A study of the bright stars. I. A catalogue of spectral classifications.". The Astronomical Journal 74: 375. doi:10.1086/110819. ISSN 0004-6256. Bibcode: 1969AJ.....74..375C. 
  7. ↑ 7.0 7.1 7.2 7.3 Abt, Helmut A.; Morrell, Nidia I. (July 1995). "The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars". The Astrophysical Journal Supplement Series 99: 135. doi:10.1086/192182. ISSN 0067-0049. Bibcode: 1995ApJS...99..135A. 
  8. ↑ 8.0 8.1 Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data. SIMBAD, Bibcode: 1986EgUBV........0M 
  9. ↑ 9.0 9.1 Schröder, C.; Schmitt, J. H. M. M. (24 September 2007). "X-ray emission from A-type stars". Astronomy & Astrophysics 475 (2): 677–684. doi:10.1051/0004-6361:20077429. ISSN 0004-6361. Bibcode: 2007A&A...475..677S. 
  10. ↑ 10.0 10.1 Wilson, Ralph Elmer (1953). "General catalogue of stellar radial velocities.". Carnegie Institute Washington D.C. Publication: 0. Bibcode: 1953GCRV..C......0W. 
  11. ↑ 11.0 11.1 Anderson, E.; Francis, Ch. (May 2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331–346. doi:10.1134/S1063773712050015. ISSN 1063-7737. Bibcode: 2012AstL...38..331A. 
  12. ↑ 12.0 12.1 Kervella, P.; Thévenin, F.; Di Folco, E.; Ségransan, D. (April 8, 2004). "The angular sizes of dwarf stars and subgiants: Surface brightness relations calibrated by interferometry". Astronomy & Astrophysics 426 (1): 297–307. doi:10.1051/0004-6361:20035930. ISSN 0004-6361. Bibcode: 2004A&A...426..297K. 
  13. ↑ Stassun, Keivan G. et al. (9 September 2019). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal 158 (4): 138. doi:10.3847/1538-3881/ab3467. Bibcode: 2019AJ....158..138S. 
  14. ↑ 14.0 14.1 Fracassini, M.; Manzolini, F.; Pasinetti, L. E.; Ruggenini, M. (May 1980). "Apparent radii and other parameters for 416 B5 V-F5 V stars of the catalogue of the Geneva observatory". Astrophysics and Space Science (Springer Science and Business Media LLC) 69 (2): 401–423. doi:10.1007/bf00661927. ISSN 0004-640X. Bibcode: 1980Ap&SS..69..401F. 
  15. ↑ 15.0 15.1 Anders, F. et al. (August 2019). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18". Astronomy & Astrophysics 628: A94. doi:10.1051/0004-6361/201935765. ISSN 0004-6361. Bibcode: 2019A&A...628A..94A. 
  16. ↑ "HD 4222". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+4222. 
  17. ↑ Eggleton, P. P.; Tokovinin, A. A. (11 September 2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society 389 (2): 869–879. doi:10.1111/j.1365-2966.2008.13596.x. ISSN 0035-8711. Bibcode: 2008MNRAS.389..869E. 
  18. ↑ Eggen, O. J. (June 1, 1960). "Stellar Groups, VIII. The Structure of the Sirius Group". Monthly Notices of the Royal Astronomical Society (Oxford University Press (OUP)) 120 (6): 563–580. doi:10.1093/mnras/120.6.563. ISSN 0035-8711. Bibcode: 1960MNRAS.120..563E. 



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