HD 133880

Last updated
HD 133880
HRLupLightCurve.png
A light curve for HR Lupi, plotted from TESS data [1]
Observation data
Epoch J2000.0        Equinox J2000.0
Constellation Lupus
Right ascension 15h 08m 12.12388s [2]
Declination −40° 35′ 02.1554″ [2]
Apparent magnitude  (V)5.76 - 5.81 [3]
Characteristics
Spectral type B8IVp Si λ4200 [4]
Variable type SX Arietis [3]
Astrometry
Proper motion (μ)RA: −28.686±0.085 [2]   mas/yr
Dec.: −31.533±0.071 [2]   mas/yr
Parallax (π)9.4922 ± 0.0786  mas [2]
Distance 344 ± 3  ly
(105.3 ± 0.9  pc)
Absolute magnitude  (MV)0.53 [5]
Details
Mass 3.20±0.15 [6]   M☉
Radius 2.01±0.32 [7]   R☉
Luminosity 105 [7]   L☉
Surface gravity (log g)4.28 [2]   cgs
Temperature 13,000±600 [7]   K
Rotational velocity (v sin i)103±10 [7]  km/s
Age 16+4
−3 [6]   Myr
Other designations
HR Lupi, HIP  74066, HR  5624, SAO  225474, [8]
Database references
SIMBAD data

HD 133880, also known as HR 5624 and HR Lupi, is a Bp star about 340 light years from the Earth, in the constellation Lupus. [2] It is a 5th magnitude star, and will be faintly visible to the naked eye of an observer far from city lights. It is an SX Arietis variable star, varying from magnitude 5.76 to 5.81 over a period of 21.0594 hours. [3] HD 133880 is a member of the Upper Centaurus–Lupus association. It is a young star, estimated to have completed only 5±2 percent of its projected main sequence lifetime. [6] It is one of the few stars known to produce coherent pulsed radio radiation via electron cyclotron maser emission. [9]

The spectrum of HD 133880 matches a B8 subgiant, but with unusually strong absorption lines of some metals, making it a member of the chemically peculiar Ap/Bp star class. For this particular star, silicon lines at 4,200  Å are notably strong. [6] Its rotation rate is unusually fast for a star of this type. [7]

In 1985, Christoffel Waelkens found that HD 133880 is a variable star with a period of 0.87746±0.00001 days, varying by 0.15, 0.10 and 0.06 magnitudes in the U, B and V bands respectively. [10] In 1986, the star was given the variable star designation HR Lupi. [11] Later measurements of the period varied significantly, and can only be reconciled if the period varies in time. [12]

In 1990, John Landstreet found that HD 133880 has a very strong (several kG) magnetic field, with the unusual property that its quadrupole term is stronger than the dipole term. [13] However a study in 2017 found the magnetic field was better described as a distorted asymmetric dipole, with a maximum strength of 12 kG, and an average strength of 4 kG. [14]

Much of the research interest in HD 133880 arises from its radio emissions. Jeremy Lim et al. observed the star with the Australia Telescope Compact Array in 1995, and found that because the star's magnetic and rotation axes are not aligned, the 6 cm wavelength radiation they measured showed variation in both strength and polarization as the star rotated. [15] In 2018 Barnali Das et al. detected electron cyclotron maser emission [16] from the star at 610 MHz, using the GMRT. HD 133880 was the second star found to radiate in this way (after CU Virginis). The radiation was found to vary by an order of magnitude as the star rotated, and had roughly 100 percent right circular polarization when the emission peaked. [12]

Related Research Articles

GY Andromedae is an α2 Canum Venaticorum type variable star in the northern constellation Andromeda. Its brightness fluctuates in visual magnitude between 6.27m and 6.41m, making it a challenge to view with the naked eye even in good seeing conditions. The magnetic activity on this star shows an unusually long period of variability, cycling about once every 23 years. Based upon parallax measurements, this star is located at a distance of about 460 light-years from the Earth.

<span class="mw-page-title-main">12 Canis Majoris</span> Variable star in the constellation Canis Major

12 Canis Majoris is a variable star located 750 light years away from the Sun in the southern constellation of Canis Major. It has the variable star designation HK Canis Majoris; 12 Canis Majoris is the Flamsteed designation. This body is just barely visible to the naked eye as a dim, blue-white hued star with a baseline apparent visual magnitude of +6.07. It is moving away from the Earth with a heliocentric radial velocity of +16 km/s. This is the brightest star in the vicinity of the open cluster NGC 2287, although it is probably not a member based on its proper motion.

<span class="mw-page-title-main">HD 125823</span> SX Arietis variable in the constellation Centaurus

HD 125823, also known as V761 Centauri or a Centauri, is a variable star in the constellation Centaurus. It is a blue-white star that is visible to the naked eye with a mean apparent visual magnitude of +4.41. The distance to this star is approximately 460 light years based on parallax measurements. It is a member of the Upper Centaurus–Lupus subgroup of the Scorpius–Centaurus association.

<span class="mw-page-title-main">BN Camelopardalis</span> Star in the constellation Camelopardalis

BN Camelopardalis is a suspected astrometric binary in the northern circumpolar constellation of Camelopardalis. It appears as a variable star that is visible to the naked eye as a dim, white-hued point of light with an apparent visual magnitude that fluctuates around 5.49. The system is located at a distance of around 310 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +9 km/s.

<span class="mw-page-title-main">VX Sagittarii</span> Extreme asymptotic giant branch star in the constellation Sagittarius

VX Sagittarii is an extreme asymptotic giant branch star located more than 1.5 kiloparsec away from the Sun in the constellation of Sagittarius. It is a pulsating variable star with an unusually large magnitude range. It is also one of the largest stars discovered so far, with a radius varying between 1,350 and 1,940 solar radii (940,000,000 and 1.35×109 km; 6.3 and 9.0 au). It is the most luminous known AGB star, at bolometric magnitude –8.6, which is even brighter than the theoretical limit at –8.0.

<span class="mw-page-title-main">V518 Carinae</span> Blue-hued variable star in the constellation Carina

V518 Carinae is a naked-eye variable star in the constellation Carina. It is a member of the bright open cluster IC 2602 near the Carina Nebula.

<span class="mw-page-title-main">HD 93194</span> Star in the constellation Carina

HD 93194 is a star in the constellation Carina. Its apparent magnitude is 4.79. Its parent cluster is IC 2602.

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

HD 93607 is a star in the constellation Carina. Its apparent magnitude is 4.87. Its parent cluster is IC 2602.

<span class="mw-page-title-main">HD 21278</span> Binary star system in the constellation Perseus

HD 21278 is a binary star system in the constellation Perseus, located within the 60±7 million year old Alpha Persei Cluster. It has a blue-white hue and is visible to the naked eye with a combined apparent visual magnitude of 4.99. The system is located at a distance of approximately 580 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +1.20 km/s.

<span class="mw-page-title-main">HD 64740</span> Blue-hued main-sequence star in the constellation Puppis

HD 64740 is a single star in the southern constellation Puppis, positioned near the line of sight to the Gum Nebula. It has a blue-white hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.63. Parallax measurements give a distance estimate of approximately 760 light-years from the Sun, and it is drifting further away with a radial velocity of +8 km/s.

<span class="mw-page-title-main">CU Virginis</span> Ap star in the constellation Virgo

CU Virginis is a single star in the equatorial constellation of Virgo. It has an apparent visual magnitude of 4.99, which is bright enough to be faintly visible to the naked eye. The distance to this star can be estimated from its annual parallax shift of 13.9 mas, yielding a separation of 234 light years.

<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">HD 137509</span> Star in the constellation Apus

HD 137509 is a star in the southern constellation of Apus, positioned less than a degree from the northern constellation boundary with Triangulum Australe. It has the variable star designation of NN Apodis, or NN Aps for short, and ranges in brightness from an apparent visual magnitude of 6.86 down to 6.93 with a period of 4.4916 days. The star is located at a distance of approximately 647 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +0.50 km/s.

<span class="mw-page-title-main">S Cassiopeiae</span> Star in the constellation Cassiopeia

S Cassiopeiae is a Mira variable and S-type star in the constellation Cassiopeia. It is an unusually cool star, rapidly losing mass and surrounded by dense gas and dust producing masers.

<span class="mw-page-title-main">BF Orionis</span> Young protostar system

BF Orionis is a young Herbig Ae/Be star in the constellation of Orion about 1250 light years away, within the Orion Nebula. It is the most massive star of the small birth cluster of four stars.

<span class="mw-page-title-main">KQ Velorum</span> Binary star system in the constellation Vela

KQ Velorum is a variable star system in the southern constellation of Vela. It has the identifier HD 94660 in the Henry Draper Catalogue; KQ Vel is the variable star designation. This appears as a sixth magnitude star with an apparent visual magnitude of 6.112, and thus is dimly visible to the naked eye under suitable viewing conditions. The system is located at a distance of approximately 373 light years from the Sun based on parallax measurements, and is drifting further away with a radial velocity of around 23 km/s.

HR 7355 is a star in the southern constellation of Sagittarius. It is faintly visible to the naked eye with an apparent visual magnitude of 6.03. The star is located at a distance of approximately 760 light years based on parallax measurements. The radial velocity of the star is poorly constrained, but it appears to be receding at the rate of +4 km/s.

<span class="mw-page-title-main">LQ Hydrae</span> Star in the constellation Hydra

LQ Hydrae is a single variable star in the equatorial constellation of Hydra. It is sometimes identified as Gl 355 from the Gliese Catalogue; LQ Hydrae is the variable star designation, which is abbreviated LQ Hya. The brightness of the star ranges from an apparent visual magnitude of 7.79 down to 7.86, which is too faint to be readily visible to the naked eye. Based on parallax measurements, this star is located at a distance of 59.6 light years from the Sun. It is drifting further away with a radial velocity of 7.6 km/s.

<span class="mw-page-title-main">HD 125248</span> Binary star system in the constellation of Virgo

HD 125248 is a binary star system in the equatorial constellation of Virgo. It has the variable star designation CS Virginis, while HD 125248 is the designation from the Henry Draper Catalogue. This system is dimly visible to the naked eye as a point of light with an apparent visual magnitude that ranges from 5.84 down to 5.95. It is located at a distance of approximately 280 light years from the Sun based on parallax measurements, but is drifting closer with a heliocentric radial velocity of −8 km/s.

<span class="mw-page-title-main">HR 1217</span> Star in the constellation Eridanus

HR 1217 is a variable star in the constellation Eridanus. It has the variable star designation DO Eridani, but this seldom appears in the astronomical literature; it is usually called either HR 1217 or HD 24712. At its brightest, HR 1217 has an apparent magnitude of 5.97, making it very faintly visible to the naked eye for an observer with excellent dark-sky conditions.

References

  1. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 22 January 2023.
  2. 1 2 3 4 5 6 7 Vallenari, A.; et al. (Gaia Collaboration) (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics . arXiv: 2208.00211 . doi: 10.1051/0004-6361/202243940 . Gaia DR3 record for this source at VizieR.
  3. 1 2 3 "HR Lup". The International Variable Star Index. AAVSO. Retrieved 22 January 2023.
  4. ↑ Bychkov, V. D.; Bychkova, L. V.; Madej, J. (August 2021). "Catalog of averaged magnetic phase curves of stars. Second edition". Astronomy and Astrophysics. 652: A31. arXiv: 2004.14099 . Bibcode:2021A&A...652A..31B. doi: 10.1051/0004-6361/202040215 .
  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. ISSN   1063-7737. S2CID   119257644.
  6. 1 2 3 4 Landstreet, J. D.; Bagnulo, S.; Andretta, V.; Fossati, L.; Mason, E.; Silaj, J.; Wade, G. A. (August 2007). "Searching for links between magnetic fields and stellar evolution: II. The evolution of magnetic fields as revealed by observations of Ap stars in open clusters and associations". Astronomy and Astrophysics. 470 (2): 685. arXiv: 0706.0330 . Bibcode:2007A&A...470..685L. doi: 10.1051/0004-6361:20077343 .
  7. 1 2 3 4 5 Bailey, J. D.; Grunhut, J.; Shultz, M.; Wade, G.; Landstreet, J. D.; Bohlender, D.; Lim, J.; Wong, K.; Drake, S.; Linsky, J.; MiMeS Collaboration (June 2012). "An analysis of the rapidly rotating Bp star HD 133880". Monthly Notices of the Royal Astronomical Society. 423 (1): 328–343. arXiv: 1203.5277 . Bibcode:2012MNRAS.423..328B. doi: 10.1111/j.1365-2966.2012.20881.x .
  8. ↑ "HR Lup -- alpha2 CVn Variable". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2023-01-22.
  9. ↑ Das, Barnali; Chandra, Poonam; Wade, Gregg A. (November 2020). "Unravelling the complex magnetosphere of the B star HD 133880 via wideband observation of coherent radio emission". Monthly Notices of the Royal Astronomical Society. 499 (1): 702–709. arXiv: 2008.07170 . Bibcode:2020MNRAS.499..702D. doi: 10.1093/mnras/staa2499 .
  10. ↑ Waelkens, C. (July 1985). "Photometric variations and period determination of eight southern CP stars". Astronomy and Astrophysics Supplement Series. 61: 127–139. Bibcode: 1985A&AS...61..127W .
  11. ↑ Kholopov, P. N.; Samus, N. N.; Kazarovets, E. V. (August 1987). "The 68th Name-List of Variable Stars" (PDF). Information Bulletin on Variable Stars. 3058 (1): 1. Bibcode:1987IBVS.3058....1K . Retrieved 23 January 2023.
  12. 1 2 Das, Barnali; Chandra, Poonam; Wade, Gregg A. (February 2018). "Discovery of electron cyclotron MASER emission from the magnetic Bp star HD 133880 with the Giant Metrewave Radio Telescope". Monthly Notices of the Royal Astronomical Society: Letters. 474 (1): L61-L65. arXiv: 1711.09836 . Bibcode:2018MNRAS.474L..61D. doi: 10.1093/mnrasl/slx193 .
  13. ↑ Landstreet, J. D. (March 1990). "The Very Strong and Unusual Magnetic Field of the BP Silicon Star HD 133880". Astrophysical Journal Letters. 352: L5. Bibcode:1990ApJ...352L...5L. doi: 10.1086/185680 .
  14. ↑ Kochukhov, O.; Silvester, J.; Bailey, J. D.; Landstreet, J. D.; Wade, G. A. (September 2017). "Magnetic field topology and chemical abundance distributions of the young, rapidly rotating, chemically peculiar star HR 5624". Astronomy and Astrophysics. 605: A13. arXiv: 1705.04966 . Bibcode:2017A&A...605A..13K. doi: 10.1051/0004-6361/201730919 .
  15. ↑ Lim, Jeremy; Drake, Stephen A.; Linsky, Jeffrey L. (1996). "Rotation Modulation of Radio Emissionfrom the Magnetic Bp Star HR 5624". Radio Emission from the Stars and the Sun ASP Conference Series. 93: 324. Bibcode: 1996ASPC...93..324L .
  16. ↑ Leto, P.; Trigilio, C.; Buemi, C. S.; Umana, G.; Ingallinera, A.; Cerrigone, L. (June 2016). "3D modelling of stellar auroral radio emission". Monthly Notices of the Royal Astronomical Society. 459 (2): 1159–1169. arXiv: 1603.02423 . Bibcode:2016MNRAS.459.1159L. doi: 10.1093/mnras/stw639 .
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.