HR 5907

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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
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]
Distance 467 ± 5  ly
(143 ± 2  pc)
Absolute magnitude  (MV)−0.17 [5]
Details
Mass 5.5±0.5 [4]   M☉
Radius 3.1±0.2 (equatorial) [4]   R☉
Luminosity 600+230
−170 [1]   L☉
Surface gravity (log g)4.200±0.053 [6]   cgs
Temperature 17000±1000 [4]   K
Rotation 0.508276+0.000015
−0.000012  d [4]
Rotational velocity (v sin i)340±18 [6]  km/s
Age 206 [7]   Myr
Other designations
V1040 Sco, HD  142184, HIP  77859, SAO  183901 [8]
Database references
SIMBAD data

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]

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Lambda Scorpii is a triple star system and the second-brightest object in the constellation of Scorpius. It is formally named Shaula; Lambda Scorpii is its Bayer designation, which is Latinised from λ Scorpii and abbreviated Lambda Sco or λ Sco. With an apparent visual magnitude of 1.62, it is one of the brightest stars in the night sky.

<span class="mw-page-title-main">13 Andromedae</span> Star in the constellation Andromeda

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<span class="mw-page-title-main">DL Crucis</span> Star in the constellation Crux

DL Crucis is a variable star in the constellation Crux.

Kappa<sup>1</sup> Apodis Star in the constellation Apus

Kappa1 Apodis, Latinized from κ1 Apodis, is the Bayer designation for a binary star system in the southern circumpolar constellation of Apus. Based upon parallax measurements, it is located roughly 1,060 light-years from Earth. The combined apparent visual magnitude of the system is 5.52, indicating that this is a faint, naked eye star that can be viewed in dark suburban skies. It is moving away from the Sun with a radial velocity of +62 km/s.

<span class="mw-page-title-main">Chi Ophiuchi</span> Star in the constellation Ophiuchus

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<span class="mw-page-title-main">HD 93607</span> Star in the constellation Carina

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f Eridani Multiple star system in the constellation Eridanus

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N Scorpii, also known as HD 148703, is a solitary, bluish-white hued star located in the southern constellation Scorpius. It has an apparent magnitude of 4.23, making it readily visible to the naked eye. N Scorpii was initially given the Bayer designation Alpha Normae by Lacaille but it was later moved from Norma to Scorpius. N Scorpii is currently located 550 light years away based on parallax measurements from the Hipparcos satellite and is part of the Upper Scorpius–Centaurus region of the Scorpius–Centaurus association.

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<span class="mw-page-title-main">Y Centauri</span> Variable star in the constellation Centaurus

Y Centauri or Y Cen is a semiregular variable star in the constellation of Centaurus.

<span class="mw-page-title-main">HR 5171</span> Star in the constellation Centaurus

V766 Centauri, also known as HR 5171, is a yellow hypergiant in the constellation Centaurus, either 5,000 or 12,000 light years from Earth. It is said to be either an extreme red supergiant (RSG) or recent post-red supergiant (Post-RSG) yellow hypergiant (YHG), both of which suggest it is one of the largest known stars. The star's diameter is uncertain but likely to be between 1,100 and 1,600 times that of the Sun. It was previously thought to be a contact binary, sharing a common envelope of material with a smaller yellow supergiant and secondary star, the two orbiting each other every 1,304 ± 6 days. However this has since been deemed unlikely. An optical companion, HR 5171B, may or may not be at the same distance as the yellow supergiant.

<span class="mw-page-title-main">V915 Scorpii</span> Variable star in the constellation Scorpius

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<span class="mw-page-title-main">V2052 Ophiuchi</span> Variable star in the constellation Ophiuchus

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<span class="mw-page-title-main">HR 2501</span> Star in the constellation Canis Major

HR 2501, also known as HD 49131 and HP Canis Majoris, is a star about 2,000 light years from the Earth, in the constellation Canis Major. It is a 5th magnitude star, so it will be faintly visible to the naked eye of an observer far from city lights. It is a variable star, whose brightness varies from magnitude 5.35 to 5.80 on a variety of timescales ranging from hours to hundreds of days.

<span class="mw-page-title-main">HD 142990</span> Star in the constellation Scorpius

HD 142990, also known as HR 5942 and V913 Scorpii, is a star about 470 light years from the Earth, in the constellation Scorpius. It is a 5th magnitude star, so it will be faintly visible to the naked eye of an observer far from city lights. It is a variable star, whose brightness varies slightly from 5.40 to 5.47 during its 23.5 hour rotation period. It is a member of the Upper Scorpius Region of the Scorpius–Centaurus association.

References

  1. 1 2 3 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 . Retrieved 18 February 2023.
  2. 1 2 3 4 5 6 7 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. 1 2 3 "V1040 Sco". The International Variable Star Index. AAVSO. Retrieved 18 February 2023.
  4. 1 2 3 4 5 6 7 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. 1 2 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. Bibcode:2014ApJS..215...10N. doi: 10.1088/0067-0049/215/1/10 . S2CID   54074229 . Retrieved 19 February 2023.
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