Astronomy:HR 5907

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Short description: Star in the constellation Scorpius
HR 5907
V1040ScoLightCurve.png
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
Equinox J2000.0]] (ICRS)
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[2] mas
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

  1. ↑ 1.0 1.1 1.2 Grunhut, J. H.; Rivinius, Th.; Wade, G. A.; Townsend, R. H. D.; Marcolino, W. L. F.; Bohlender, D. A.; Szeifert, Th.; Petit, V. et al. (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. doi:10.1111/j.1365-2966.2011.19824.x. Bibcode: 2012MNRAS.419.1610G. https://academic.oup.com/mnras/article/419/2/1610/989444. Retrieved 18 February 2023. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 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.
  3. ↑ 3.0 3.1 3.2 "V1040 Sco". AAVSO. https://www.aavso.org/vsx/index.php?view=detail.top&oid=33856. 
  4. ↑ 4.0 4.1 4.2 4.3 4.4 4.5 4.6 Leto, P.; Trigilio, C.; Oskinova, L. M.; Ignace, R.; Buemi, C. S.; Umana, G.; Ingallinera, A.; Leone, F. et al. (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. doi:10.1093/mnras/sty244. Bibcode: 2018MNRAS.476..562L. https://academic.oup.com/mnras/article/476/1/562/4832493. Retrieved 19 February 2023. 
  5. ↑ 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. 
  6. ↑ 6.0 6.1 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. doi:10.1051/0004-6361:20042229. Bibcode: 2005A&A...440..305F. https://www.aanda.org/component/article?access=bibcode&bibcode=&bibcode=2005A%2526A...440..305FFUL. 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. doi:10.1134/S1063773712120031. ISSN 1063-7737. Bibcode: 2012AstL...38..771G. 
  8. ↑ "HD 142184 -- Be Star". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+142184+--+Be+Star. 
  9. ↑ Bertiau, F. C. (November 1958). "Absolute Magnitudes of Stars in the Scorpio-Centaurus Association". Astrophysical Journal 128: 533–561. doi:10.1086/146569. Bibcode: 1958ApJ...128..533B. 
  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. doi:10.1093/mnras/121.3.263. Bibcode: 1960MNRAS.121..263B. https://academic.oup.com/mnras/article/121/3/263/2601309. Retrieved 18 February 2023. 
  11. ↑ Graham, Hill (August 1967). "Some New Variables in Nearby Associations and Galactic Clusters". Astrophysical Journal Supplement 14: 301–306. doi:10.1086/190157. Bibcode: 1967ApJS...14..301H. 
  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. https://ui.adsabs.harvard.edu/abs/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". Information Bulletin on Variable Stars 4659 (1). Bibcode: 1999IBVS.4659....1K. https://ibvs.konkoly.hu/pub/ibvs/4601/4659.pdf. 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. doi:10.1088/0067-0049/215/1/10. Bibcode: 2014ApJS..215...10N. https://iopscience.iop.org/article/10.1088/0067-0049/215/1/10. Retrieved 19 February 2023. 



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