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HR 5907

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HR 5907

A light curve for V1040 Scorpii, adapted from Grunhut et al. (2012).[1] The data is from MOST but has been shifted to match the Hipparcos magnitude scale.
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Scorpius
Right ascension 15h 53m 55.86379s[2]
Declination −23° 58′ 41.1434″[2]
Apparent magnitude (V) 5.39 - 5.43[3]
Characteristics
Spectral type B2.5V[4]
Variable type SX Ari[3]
Astrometry
Proper motion (μ) RA: −13.406±0.083[2] mas/yr
Dec.: −24.111±0.064[2] mas/yr
Parallax (π)6.9899 ± 0.0739 mas[2]
Distance467 ± 5 ly
(143 ± 2 pc)
Absolute magnitude (MV)−0.17[5]
Details
Mass5.5±0.5[4] M☉
Radius3.1±0.2 (equatorial)[4] R☉
Luminosity600+230
−170[1] L☉
Surface gravity (log g)4.200±0.053[6] cgs
Temperature17000±1000[4] K
Rotation0.508276+0.000015
−0.000012 d[4]
Rotational velocity (v sin i)340±18[6] km/s
Age206[7] Myr
Other designations
V1040 Sco, HD 142184, HIP 77859, SAO 183901[8]
Database references
SIMBADdata

HR 5907, also known as V1040 Scorpii and HD 142184, is a star about 470 light years from the Earth, in the constellation Scorpius.[2] It is a 5th magnitude star, so it will be faintly visible to the naked eye of an observer far from city lights.[2] Its brightness varies slightly, ranging from magnitude 5.39 to 5.43 every 12 hours and 20 minutes.[3] HR 5907 is a member of the Scorpius–Centaurus association.[9]

Spectroscopic observations by William Buscombe and Pamela Morris during the years 1956 through 1959 showed that the radial velocity of HR 5907 varied by about 50 km/sec.[10] In 1966, Graham Hill first detected brightness variations in HD 5907. He determined that the brightness varied by 0.03 magnitudes, but was unable to classify the star's type of variability.[11] In 1998, Anne Marie Hubert and Michele Floquet examined the Hipparcos data for the star, confirmed that its brightness varies, and derived a period of 0.508 days with no indications of long-term variability.[12] In 1996 HR 5907 was given the variable star designation V1040 Scorpii.[13]

As of 2018, HR 5907 was the most luminous early spectral type star known at centimeter and millimeter radio wavelengths. [4] On the other end of the electromagnetic spectrum, in 2012 it was clearly detected by the Chandra X-ray Observatory.[14]

HR 5907 is a main sequence star with a strong magnetic field. As of 2018, it had the shortest rotation period known of any early spectral type magnetic star. It spins so rapidly that the star's polar radius is only 88% as large as the equatorial radius.[4] The star has a dipole magnetic field strength of at least 10 kilogauss.[1]

References

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  1. ^ a b c Grunhut, J. H.; Rivinius, Th.; Wade, G. A.; Townsend, R. H. D.; Marcolino, W. L. F.; Bohlender, D. A.; Szeifert, Th.; Petit, V.; Matthews, J. M.; Rowe, J. F.; Moffat, A. F. J.; Kallinger, T.; Kuschnig, R.; Guenther, D. B.; Rucinski, S. M.; Sasselov, D.; Weiss, W. W. (January 2012). "HR 5907: Discovery of the most rapidly rotating magnetic early B-type star by the MiMeS Collaboration". Monthly Notices of the Royal Astronomical Society. 419 (2): 1610–1627. arXiv:1109.3157. Bibcode:2012MNRAS.419.1610G. doi:10.1111/j.1365-2966.2011.19824.x. S2CID 59038744.
  2. ^ a b c d e f g 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.
  3. ^ a b c "V1040 Sco". The International Variable Star Index. AAVSO. Retrieved 18 February 2023.
  4. ^ a b c d e f g Leto, P.; Trigilio, C.; Oskinova, L. M.; Ignace, R.; Buemi, C. S.; Umana, G.; Ingallinera, A.; Leone, F.; Phillips, N. M.; Agliozzo, C.; Todt, H.; Cerrigone, L. (May 2018). "A combined multiwavelength VLA/ALMA/Chandra study unveils the complex magnetosphere of the B-type star HR5907". Monthly Notices of the Royal Astronomical Society. 476 (1): 562–579. arXiv:1801.08738. Bibcode:2018MNRAS.476..562L. doi:10.1093/mnras/sty244. Retrieved 19 February 2023.
  5. ^ Anderson, E.; Francis, Ch. (May 2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331–346. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. eISSN 1562-6873. ISSN 1063-7737. S2CID 119257644.
  6. ^ a b Frémat, Y.; Zorec, J.; Hubert, A. M.; Floquet, M. (September 2005). "Effects of gravitational darkening on the determination of fundamental parameters in fast-rotating B-type stars". Astronomy and Astrophysics. 440 (1): 305–320. arXiv:astro-ph/0503381. Bibcode:2005A&A...440..305F. doi:10.1051/0004-6361:20042229. S2CID 19016751. Retrieved 19 February 2023.
  7. ^ Gontcharov, G. A. (December 2012). "Dependence of kinematics on the age of stars in the solar neighborhood". Astronomy Letters. 38 (12): 771–782. arXiv:1606.08814. Bibcode:2012AstL...38..771G. doi:10.1134/S1063773712120031. eISSN 1562-6873. ISSN 1063-7737.
  8. ^ "HD 142184 -- Be Star". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2023-02-18.
  9. ^ Bertiau, F. C. (November 1958). "Absolute Magnitudes of Stars in the Scorpio-Centaurus Association". Astrophysical Journal. 128: 533–561. Bibcode:1958ApJ...128..533B. doi:10.1086/146569.
  10. ^ Buscombe, W.; Morris, P. M. (1960). "The Scorpio-Centaurus association: I. Radial velocities of 120 bright stars". Monthly Notices of the Royal Astronomical Society. 121 (3): 263–278. Bibcode:1960MNRAS.121..263B. doi:10.1093/mnras/121.3.263. Retrieved 18 February 2023.
  11. ^ Graham, Hill (August 1967). "Some New Variables in Nearby Associations and Galactic Clusters". Astrophysical Journal Supplement. 14: 301–306. Bibcode:1967ApJS...14..301H. doi:10.1086/190157.
  12. ^ Hubert, A. M.; Floquet, M. (July 1998). "Investigation of the variability of bright Be stars using HIPPARCOS photometry". Astronomy and Astrophysics. 335: 565–572. Bibcode:1998A&A...335..565H. Retrieved 19 February 2023.
  13. ^ Kazarovets, E. V.; Samus, N. N.; Durlevich, O. V.; Frolov, M. S.; Antipin, S. V.; Kireeva, N. N.; Pastukhova, E. N. (January 1999). "The 74th Special Name-list of Variable Stars" (PDF). Information Bulletin on Variable Stars. 4659 (1). Bibcode:1999IBVS.4659....1K. Retrieved 19 February 2023.
  14. ^ Nazé, Yaël; Petit, Véronique; Rinbrand, Melanie; Cohen, David; Owocki, Stan; ud-Doula, Asif; Wade, Gregg A. (November 2014). "X-Ray Emission from Magnetic Massive Stars". The Astrophysical Journal Supplement. 215 (1): 10. arXiv:1409.1690. Bibcode:2014ApJS..215...10N. doi:10.1088/0067-0049/215/1/10. S2CID 54074229.
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