Jump to content

HD 43317

Edit links
From Wikipedia, the free encyclopedia
HD 43317
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Orion
Right ascension 06h 15m 47.013s[1]
Declination +04° 17′ 01.10″[1]
Apparent magnitude (V) 6.63[2]
Characteristics
Evolutionary stage Main sequence[3]
Spectral type B3.5 V[3] or B3 IV[4]
U−B color index −0.646[2]
B−V color index −0.164±0.010[2]
Variable type SPB/β Cep hybrid[5]
Astrometry
Radial velocity (Rv)13.0±4.4[6] km/s
Proper motion (μ) RA: −4.231 mas/yr[1]
Dec.: −3.765 mas/yr[1]
Parallax (π)3.0975 ± 0.0517 mas[1]
Distance1,050 ± 20 ly
(323 ± 5 pc)
Absolute magnitude (MV)−1.13[2]
Details
Mass5.8+0.1
−0.2[3] M☉
Radius3.39[7] R☉
Luminosity737.5[2] L☉
Surface gravity (log g)4.0±0.1[3] cgs
Temperature17,350±750[3] K
Rotation0.897673(4) d[3]
Rotational velocity (v sin i)115±9[3] km/s
Age28.4[7] Myr
Other designations
CoRoT 3412, BD+04° 1181, FK5 2478, HD 43317, HIP 29739, HR 2232, SAO 113653, PPM 150182[8]
Database references
SIMBADdata

HD 43317 is a variable star in the equatorial constellation of Orion, the hunter. It has an apparent visual magnitude of 6.63,[2] which is faint enough to be a challenge to view with the naked eye under good conditions. Based on parallax measurements, it is located at a distance of approximately 1,050 light years from the Sun. It is drifting further away with a heliocentric radial velocity of about 13 km/s.[6] This star is a member of an open cluster designated OCSN 63.[9]

Observations

[edit]

During 2009–2010, HD 43317 was observed by the CoRoT space telescope during the LRa03 (long run) sequence for asteroseismological purposes. This program lasted for a period of 150.41 days, during which the star was under almost constant observation. After being combined with HARPS data, the star was classified as a hybrid slowly pulsating B-type star and a Beta Cephei variable. Both g (gravity) and p (pressure) mode pulsations were detected. It is spinning rapidly at about half of its critical velocity.[10]

The photometry and spectrometry of HD 43317 showed rotational modulation of regions with temperature or chemical differences. These are an indirect indicator of a magnetic field. In addition, X-ray emission was detected by ROSAT, which also suggests a potential magnetic field. A magnetic field was directly detected with the Téléscope Bernard Lyot during 2012. The longitudinal field strength was found to vary with the 21.5 h rotation period, ranging from −140 G to 180 G.[11] Modelling of the star's dipolar field found a strength between 1 and 1.5 kG. This is strong enough to force uniform rotation in the outer radiative zone of the star.[5]

The CoRot light curve of the star displays 35 different frequencies, of which 28 are not related to the rotation period. Seismic modeling of the star determined a stellar mass equal to 5.8 times the mass of the Sun. At the core, the central mass fraction of hydrogen is 54%, compared to 70% for a newly formed main sequence star and 0.1% at the end of main sequence lifetime. Spectroscopic analysis shows an effective temperature of around 17,350 in the stellar atmosphere. A refined estimate of the surface magnetic field strength found a value of 1,312±332 G.[12] The magnetic field near the core has a seismically modelled strength of 5×105 G. HD 43317 is the first main sequence star for which an interior magnetic field strength has been inferred.[3]

This star has an estimated radius of 3.39 times the girth of the Sun,[7] and is radiating 737.5[2] times the Sun's luminosity. It is about 28.4 million years old.[7]

References

[edit]
  1. ^ a b c d Vallenari, 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 at VizieR.
  2. ^ a b c d e f g 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.
  3. ^ a b c d e f g h Lecoanet, Daniel; et al. (May 2022), "Asteroseismic inference of the near-core magnetic field strength in the main-sequence B star HD 43317", Monthly Notices of the Royal Astronomical Society: Letters, 512 (1): L16–L20, arXiv:2202.03440, Bibcode:2022MNRAS.512L..16L, doi:10.1093/mnrasl/slac013.
  4. ^ Lesh, Janet Rountree (December 1968), "The Kinematics of the Gould Belt: an Expanding Group?", Astrophysical Journal Supplement, 17: 371, Bibcode:1968ApJS...17..371L, doi:10.1086/190179.
  5. ^ a b Buysschaert, B.; et al. (September 2017), "Magnetic characterization of the SPB/β Cep hybrid pulsator HD 43317", Astronomy & Astrophysics, 605, id. A104, arXiv:1707.09148, Bibcode:2017A&A...605A.104B, doi:10.1051/0004-6361/201731012.
  6. ^ a b Gontcharov, G. A. (2006), "Pulkovo compilation of radial velocities for 35495 stars in a common system", Astronomy Letters, 32 (11): 759–771, arXiv:1606.08053, Bibcode:2006AstL...32..759G, doi:10.1134/S1063773706110065, S2CID 119231169.
  7. ^ a b c d Prat, V.; et al. (April 2020), "Period spacings of gravity modes in rapidly rotating magnetic stars. II. The case of an oblique dipolar fossil magnetic field", Astronomy & Astrophysics, 636, id. A100, arXiv:2003.08218, Bibcode:2020A&A...636A.100P, doi:10.1051/0004-6361/201937398.
  8. ^ "HD 43317", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2024-12-18.
  9. ^ Qin, Songmei; et al. (March 2023), "Hunting for Neighboring Open Clusters with Gaia DR3: 101 New Open Clusters within 500 pc", The Astrophysical Journal Supplement Series, 265 (1), id. 12, arXiv:2212.11034, Bibcode:2023ApJS..265...12Q, doi:10.3847/1538-4365/acadd6.
  10. ^ Pápics, P. I.; et al. (June 2012), "Gravito-inertial and pressure modes detected in the B3 IV CoRoT target HD 43317", Astronomy & Astrophysics, 542, id. A55, arXiv:1203.5231, Bibcode:2012A&A...542A..55P, doi:10.1051/0004-6361/201218809.
  11. ^ Briquet, M.; et al. (September 2013), "Discovery of a magnetic field in the CoRoT hybrid B-type pulsator HD 43317", Astronomy & Astrophysics, 557, id. L16, arXiv:1308.4636, Bibcode:2013A&A...557L..16B, doi:10.1051/0004-6361/201321779.
  12. ^ Buysschaert, B.; et al. (August 2018), "Forward seismic modeling of the pulsating magnetic B-type star HD 43317", Astronomy & Astrophysics, 616, id. A148, arXiv:1805.00802, Bibcode:2018A&A...616A.148B, doi:10.1051/0004-6361/201832642.
Retrieved from "https://wiki.riteme.site/w/index.php?title=HD_43317&oldid=1263976889"