HD 110432

Last updated
HD 110432
Crux constellation map.png
Red circle.svg
Location of BZ Crucis (circled). The other star shown overlapping/underlying the dark nebula is HD 109000 (HR 4771) which is a red/brown star about half the distance to the nebula, having parallax of 12.8 ± 0.05 thus about 250 light years away [1]
Observation data
Epoch J2000       Equinox J2000
Constellation Crux
Right ascension 12h 42m 50.2656s [1]
Declination −63° 03′ 31.048″ [1]
Apparent magnitude  (V)5.24 - 5.45 [2]
Characteristics
Spectral type B1IVe [3]
U−B color index −0.82 [4]
B−V color index +0.27 [4]
Variable type γ Cas [2]
Astrometry
Radial velocity (Rv)+35 [5]  km/s
Proper motion (μ)RA: −12.512 [1]   mas/yr
Dec.: −3.984 [1]   mas/yr
Parallax (π)2.3834 ± 0.1228  mas [1]
Distance 1,370 ± 70  ly
(420 ± 20  pc)
Absolute magnitude  (MV)−2.56 [6]
Details
Mass 9.6 [3]   M☉
Radius 6.5±1.2 [7]   R☉
Luminosity 1,153 [1]   L☉
Surface gravity (log g)3.5–3.9 [3]   cgs
Temperature 22,510–25,000 [3]   K
Rotational velocity (v sin i)300–400 [3]  km/s
Other designations
BZ Cru, HR 4830, CD-62 671, HD 110432, GCTP, SAO 252002, FK5 3015, HIP 62027. [8]
Database references
SIMBAD data
BZ Crucis is the bright star between the open clusters NGC 4609 and Hogg 15 NGC 4609 large.png
BZ Crucis is the bright star between the open clusters NGC 4609 and Hogg 15

HD 110432 is a Be star in the south-east of Crux, behind the center of the southern hemisphere's dark Coalsack Nebula. It has a stellar classification of B1IVe, which means it is a subgiant star of class B that displays emission lines in its spectrum. This is a variable star of the Gamma Cassiopeiae type, indicating it is a shell star with a circumstellar disk of gas about the equator, and has the variable star designation BZ Crucis. It is not known to be a member of a binary system, although it is probably a member of the open cluster NGC 4609. This star is moderately luminous in the X-ray band, with a variable energy emission of 1032–33 erg s−1 in the range 0.2−12 keV. The X-ray emission may be caused by magnetic activity, or possibly by accretion onto a white dwarf companion. [3]

A visual band light curve for BZ Crucis, adapted from Sarty et al. (2011) BZCruLightCurve.png
A visual band light curve for BZ Crucis, adapted from Sarty et al. (2011)

Distance

The distance of 388  pc published in the 2007 new Hipparcos reduction is over twice the distance of the Coalsack Nebula. [10] The distance from Gaia Data Release 2 is even further at 420 pc. [1]

Related Research Articles

R Apodis is a star in the constellation Apus.

HD 113703, also known by the Bayer designation f Centauri, is a multiple star system in the southern constellation of Centaurus. The combined apparent visual magnitude of this system is +4.71, which is sufficient to make it faintly visible to the naked eye. The distance to this system is approximately 400 light years based on parallax measurements. It is a member of the Lower Centaurus Crux subgroup of the Scorpius–Centaurus association.

LS I +61 303 is a microquasar, a binary system containing a massive star and a compact object. The compact object is a pulsar and the system is around 7,000 light-years away.

<span class="mw-page-title-main">R Coronae Australis</span> Star in the constellation Corona Australis

R Coronae Australis is a variable binary system in the constellation Corona Australis. It has varied between magnitudes 10 and 14.36. A small reflection/emission nebula NGC 6729 extends from the star towards SE. It is also the brightest feature of the Coronet Cluster, therefore sometimes called R CrA Cluster.

<span class="mw-page-title-main">V385 Andromedae</span> Star in the constellation Andromeda

V385 Andromedae is a variable star in the constellation Andromeda, about 360 parsecs (1,200 ly) away. It is a red giant over a hundred times larger than the sun. It has an apparent magnitude around 6.4, just about visible to the naked eye in ideal conditions.

<span class="mw-page-title-main">PU Aurigae</span> Star in the constellation Auriga

PU Aurigae is an irregular variable star located in the constellation Auriga. A red giant, it varies by 0.1 magnitude around magnitude 5.64. Located around 560 light-years distant, it shines with a luminosity approximately 1,523 times that of the Sun and has a surface temperature of 3,482 K.

<span class="mw-page-title-main">HD 123657</span> Star in the constellation Boötes

HD 123657, or BY Boötis, is a variable star of magnitude 4.98–5.33V. This makes it a dim naked eye star. The star is located near the end of the handle of the Big Dipper, but just within the boundaries of the constellation Boötes.

<span class="mw-page-title-main">V4381 Sagittarii</span> Star in the constellation Sagittarius

V4381 Sagittarii is a variable star in the constellation Sagittarius. A white supergiant of spectral type A2/A3Iab, it is an Alpha Cygni variable that varies between apparent photographic magnitudes 6.57 and 6.62. Its visual apparent magnitude is about 6.54.

<span class="mw-page-title-main">HD 168607</span> Star in the constellation Sagittarius

HD 168607 is a blue hypergiant and luminous blue variable (LBV) star located in the constellation of Sagittarius, easy to see with amateur telescopes. It forms a pair with HD 168625, also a blue hypergiant and possible luminous blue variable, that can be seen at the south-east of M17, the Omega Nebula.

HD 91496 is a giant star in the constellation Carina, with an apparent magnitude is 4.92 and an MK spectral class of K4/5 III. It has been suspected of varying in brightness, but this has not been confirmed.

<span class="mw-page-title-main">HY Velorum</span> Star in the constellation Vela

HY Velorum is a binary star system in the southern constellation of Vela. It is a dim star but visible to the naked eye with an apparent visual magnitude of 4.83. The distance to this system, as estimated from its annual parallax shift of 7.1 mas, is 460 light years. HY Vel most likely forms a gravitationally bound pair with the magnitude 5.45 binary system KT Vel ; both are members of the IC 2391 open cluster. As of 1998, HY Vel and KT Vel had an angular separation of 76.1″ along a position angle of 311°.

<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">47 Capricorni</span> Star in the constellation Capricornus

47 Capricorni is a variable star located around 1,170 light years from the Sun in the southern constellation Capricornus, near the northern border with Aquarius. It has the variable star designation of AG Capricorni and a Bayer designation of c2 Capricorni; 47 Capricorni is the Flamsteed designation. This object is visible to the naked eye as a dim, red-hued point of light with an apparent visual magnitude that varies between 5.90 and 6.14. The star is receding from the Earth with a heliocentric radial velocity of +20 km/s.

<span class="mw-page-title-main">Gliese 908</span> Star in the constellation Pisces

Gliese 908 is a red dwarf star, located in constellation Pisces at 19.3 light-years from Earth. It is a BY Draconis variable star with a variable star designation of BR Piscium. Its apparent magnitude varies between magnitude 8.93 and magnitude 9.03 as a result of starspots and varying chromospheric activity.

<span class="mw-page-title-main">CD Crucis</span> Eclipsing binary star system in the constellation Crux

CD Crucis, also known as HD 311884, is an eclipsing binary star system in the constellation Crux. It is around 14,000 light years away near the faint open cluster Hogg 15. The binary contains a Wolf–Rayet star and is also known as WR 47.

<span class="mw-page-title-main">HD 65750</span> Star in the constellation Carina

HD 65750, also known as V341 Carinae is a bright red giant star in the constellation Carina. It is surrounded by a prominent reflection nebula, known as IC 2220, nicknamed the Toby Jug Nebula.

<span class="mw-page-title-main">V419 Cephei</span> Star in the constellation Cepheus

V419 Cephei is an irregular variable star in the constellation of Cepheus with an apparent magnitude that varies between 6.54 and 6.89.

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

DU Crucis is a red supergiant and slow irregular variable star in the open cluster NGC 4755, which is also known as the Kappa (κ) Crucis Cluster or Jewel Box Cluster.

<span class="mw-page-title-main">HD 151932</span> Star in the constellation of Scorpius

HD 151932, also known as WR 78, is a Wolf-Rayet star located in the constellation Scorpius, close to the galactic plane. Its distance is around 1,300 parsecs away from the Earth. Despite being a blue-colored Wolf-Rayet star, it is extremely reddened by interstellar extinction, so its apparent magnitude is brighter for longer-wavelength passbands. HD 151932 lies about 22′ west of the open cluster NGC 6231, the center of the OB association Scorpius OB1; it is not clear whether it is a part of the association or not. With an apparent magnitude of about 6.5, it is one of the few Wolf-Rayet stars that can be seen with the naked eye.

<span class="mw-page-title-main">Iota Mensae</span> Star in the constellation Mensa

Iota Mensae is a single star about 880 light years away in the faint constellation Mensa. It has a very slightly variable apparent magnitude of 6.0, making it visible with the naked eye under good skies.

References

  1. 1 2 3 4 5 6 7 8 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
  2. 1 2 Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1: B/gcvs. Bibcode:2009yCat....102025S.
  3. 1 2 3 4 5 6 Lopes de Oliveira, R.; et al. (November 2007). "On the X-ray and optical properties of the Be star HD 110432: a very hard-thermal X-ray emitter". Astronomy and Astrophysics. 474 (3): 983–996. arXiv: astro-ph/0701767 . Bibcode:2007A&A...474..983L. doi:10.1051/0004-6361:20077295. S2CID   14593244.
  4. 1 2 Cousins, A. W. J. (1973). "UBV photometry of some southern stars". Monthly Notes of the Astronomical Society of Southern Africa. 32: 11. Bibcode:1973MNSSA..32...11C.
  5. ↑ Evans, D. S. (June 20–24, 1966). "The Revision of the General Catalogue of Radial Velocities". In Batten, Alan Henry; Heard, John Frederick (eds.). Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30. University of Toronto: International Astronomical Union. Bibcode:1967IAUS...30...57E.
  6. ↑ 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.
  7. ↑ Stee, Ph; Meilland, A.; Bendjoya, Ph.; Millour, F.; Smith, M.; Spang, A.; Duvert, G.; Hofmann, K. -H.; Massi, F. (2013). "Evidence of an asymmetrical Keplerian disk in the Brγ and He I emission lines around the be star HD 110432". Astronomy and Astrophysics. 550: A65. arXiv: 1301.2877 . Bibcode:2013A&A...550A..65S. doi:10.1051/0004-6361/201220302. S2CID   11256230.
  8. ↑ "HR 4830 -- Be Star". SIMBAD. Centre de Données astronomiques de Strasbourg . Retrieved 2010-12-09.
  9. ↑ Sarty, Gordon E.; Pilecki, Bogumil; Reichart, Daniel E.; Ivarsen, Kevin M.; Haislip, Joshua B.; Nysewander, Melissa C.; LaCluyze, Aaron P.; Johnston, Helen M.; Shobbrook, Robert R.; Kiss, László L.; Wu, Kinwah (August 2011). "Photometric observations of three high mass X-ray binaries and a search for variations induced by orbital motion". Research in Astronomy and Astrophysics. 11 (8): 947–964. arXiv: 1105.2025 . Bibcode:2011RAA....11..947S. doi:10.1088/1674-4527/11/8/007. S2CID   250669202 . Retrieved 17 December 2021.
  10. ↑ Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv: 0708.1752 . Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID   18759600.
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.