HD 93403

Last updated
HD 93403
Observation data
Epoch J2000       Equinox J2000
Constellation Carina
Right ascension 10h 45m 44.11931s [1]
Declination −59° 24 28.1431 [1]
Apparent magnitude  (V)7.272 [2]
Characteristics
Spectral type O5.5III(fc)var [3] (O5.5I + O7V [4] )
U−B color index 0.747 [2]
B−V color index +0.212 [2]
Astrometry
Radial velocity (Rv)14.80 km/s
Proper motion (μ)RA: -7.27  mas/yr
Dec.: 2.45  mas/yr
Parallax (π)1.22 ± 0.45  mas [1]
Distance 3,200 [4]   pc
Orbit [5]
Period (P)15.093 days
Semi-major axis (a)121 R
Eccentricity (e)0.234
Inclination (i)~31°
Semi-amplitude (K1)
(primary)
79.3 km/s
Semi-amplitude (K2)
(secondary)
139.0 km/s
Details [4]
Primary
Mass 68.5 [5]   M
Radius 24  R
Luminosity 1,050,000  L
Temperature 39,300  K
Secondary
Mass 37.3 [5]   M
Radius 10  R
Luminosity257,000  L
Temperature 40,100  K
Other designations
HD  93403, HIP  52628, CD 58°3545, 2MASS J10454411-5924281, GSC 08626-00641, TYC 8626-641-1
Database references
SIMBAD data

HD 93403 is a spectroscopic binary containing two highly luminous hot blue stars. It is 10,000 light years away in the Carina Nebula in the constellation Carina. It appears to have spectral type O5.5III, but this is composed of two spectra from a blue supergiant and blue main sequence star of spectral type O5.5I and O7V respectively. The two stars orbit every 15 days with a separation that varies from 93 R to 149 R. The binary is shedding mass at the high rate of 0.0005 M per year. [3]

HD 93403 exhibits the Struve-Sahade effect, where the strength of the spectral lines of the individual components varies during the orbit. It also has colliding stellar winds that produce variable x-ray [6] and non-thermal radio emission. [7]

See also

Related Research Articles

<span class="mw-page-title-main">HD 93129</span> Triple star system in the constellation Carina

HD 93129 is a triple star system in the Carina Nebula, with all three components being hot O class stars amongst the most luminous stars in the Milky Way. It is the dominant member of the Trumpler 14 star cluster, a young star cluster within the Carina OB1 stellar association that harbors other super-luminous stars, like Eta Carinae and WR 25.

<span class="mw-page-title-main">HD 93205</span> Star system in the constellation Carina

HD 93205, or V560 Carinae, is a binary stellar system, in the Carina Nebula in the constellation Carina. It consists of two massive O-stars that revolve around each other in 6 days.

<span class="mw-page-title-main">WR 136</span> Star in the constellation of Cygnus

WR 136 is a Wolf–Rayet star located in the constellation Cygnus. It is in the center of the Crescent Nebula. Its age is estimated to be around 4.7 million years and it is nearing the end of its life. Within a few hundred thousand years, it is expected to explode as a supernova.

<span class="mw-page-title-main">HD 93250</span> Highly luminous binary star system in the constellation Carina

HD 93250 is a highly luminous hot blue binary star in the Carina Nebula in the constellation Carina.

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

AO Cassiopeiae, also known as Pearce's Star, is a binary system composed of an O8 main sequence star and an O9.2 bright giant that respectively weigh anywhere between 20.30 and 57.75 times and 14.8 and 31.73 times the mass of the Sun.

<span class="mw-page-title-main">Cygnus OB2-8A</span> Spectroscopic binary star near the center of Cygnus OB2

Cygnus OB2 #8A is a double-lined spectroscopic binary located near the centre of the Cygnus OB2 association located 5,500 light years away.

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

S Monocerotis, also known as 15 Monocerotis, is a massive multiple and variable star system located in the constellation Monoceros. It is the brightest star in the Christmas Tree open cluster in the area catalogued as NGC 2264.

<span class="mw-page-title-main">WR 22</span> Binary star in the constellation Carina

WR 22, also known as V429 Carinae or HR 4188, is an eclipsing binary star system in the constellation Carina. The system contains a Wolf-Rayet (WR) star that is one of the most massive and most luminous stars known, and is also a bright X-ray source due to colliding winds with a less massive O class companion. Its eclipsing nature and apparent magnitude make it very useful for constraining the properties of luminous hydrogen-rich WR stars.

<span class="mw-page-title-main">9 Sagittarii</span> Star in the constellation Sagittarius

9 Sagittarii is a massive binary star in the constellation Sagittarius. It has an apparent magnitude of 5.97. Both components are highly luminous O-type main-sequence stars.

<span class="mw-page-title-main">WR 46</span> Star in the constellation Crux

WR 46 is a Wolf-Rayet star in the constellation of the Southern Cross of apparent magnitude +10.8. It is located at 55 arcmin north of Theta2 Crucis. The star is a member of the distant stellar association Cru OB4, and is around 2,900 parsecs or 9,300 light years from the Solar System.

<span class="mw-page-title-main">WR 25</span> Binary star system in the constellation Carina

WR 25 is a binary star system in the turbulent star-forming region the Carina Nebula, about 6,800 light-years from Earth. It contains a Wolf-Rayet star and a hot luminous companion and is a member of the Trumpler 16 cluster. The name comes from the Catalogue of Galactic Wolf–Rayet Stars.

<span class="mw-page-title-main">R136c</span> Star in the constellation Dorado

R136c is a star located in R136, a tight knot of stars at the centre of NGC 2070, an open cluster weighing 450,000 solar masses and containing 10,000 stars. At 142 M and 3.8 million L, it is the one of the most massive stars known and one of the most luminous, along with being one of the hottest, at over 40,000 K. It was first resolved and named by Feitzinger in 1980, along with R136a and R136b.

<span class="mw-page-title-main">BI 253</span> O-type main sequence star in the constellation Dorado

BI 253 is an O2V star in the Large Magellanic Cloud and is a primary standard of the O2 type. It is one of the hottest main-sequence stars known and one of the most-massive and most-luminous stars known.

<span class="mw-page-title-main">Trumpler 16</span> Massive open cluster in the constellation Carina

Trumpler 16 is a massive open cluster that is home to some of the most luminous stars in the Milky Way galaxy. It is situated within the Carina Nebula complex in the Carina–Sagittarius Arm, located approximately 9,270 ly (2,842 pc) from Earth. The cluster has one star visible to the naked eye from the tropics southward, Eta Carinae.

<span class="mw-page-title-main">Melnick 34</span> Binary star in the Large Magellanic cloud

Melnick 34, also called BAT99-116, is a binary Wolf–Rayet star near R136 in the 30 Doradus complex in the Large Magellanic Cloud. Both components are amongst the most massive and most luminous stars known, and the system is the most massive known binary system.

<span class="mw-page-title-main">HD 15558</span> Star in the constellation Cassiopeia

HD 15558 is a massive O-type multiple star system in Cassiopeia and is specifically in our galaxy's Heart Nebula in open cluster IC 1805. The primary is a very massive star with 152 M and 660,000 L.

<span class="mw-page-title-main">WR 30a</span> Binary star in the constellation Carina

WR 30a is a massive spectroscopic binary in the constellation Carina. The primary is an extremely rare star on the WO oxygen sequence and the secondary a massive class O star. It appears near the Carina Nebula but is much further away.

<span class="mw-page-title-main">R145</span> Binary star in the constellation Dorado

R145 is a spectroscopic binary star in the Tarantula Nebula in the Large Magellanic Cloud located in the constellation Dorado. Both components are amongst the most luminous known.

<span class="mw-page-title-main">HD 149404</span> Variable star in the constellation Scorpius

HD 149404, also known as HR 6164 and V918 Scorpii, is a star about 4,300 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 rotating ellipsoidal variable, a binary star for which the two stars' combined brightness varies slightly, from magnitude 5.42 to 5.50, during their 9.8 day orbital period. It is one of the brightest members of the Ara OB1 association, which has the open cluster NGC 6193 at its center.

References

  1. 1 2 3 van Leeuwen, Floor (13 August 2007). "Validation of the new Hipparcos reduction". Astronomy & Astrophysics. 474 (2): 653–664. arXiv: 0708.1752 . Bibcode:2007A&A...474..653V. doi: 10.1051/0004-6361:20078357 . eISSN   1432-0746. ISSN   0004-6361.
  2. 1 2 3 Maíz-Apellániz, Jesús; Walborn, Nolan R.; Galué, Héctor Á.; Wei, Lisa H. (2004). "A Galactic O Star Catalog". The Astrophysical Journal Supplement Series. 151 (1): 103–148. arXiv: astro-ph/0311196 . Bibcode:2004ApJS..151..103M. doi:10.1086/381380. S2CID   118813863.
  3. 1 2 Sota, A.; Maíz Apellániz, J.; Morrell, N. I.; Barbá, R. H.; Walborn, N. R.; Gamen, R. C.; Arias, J. I.; Alfaro, E. J. (2014). "The Galactic O-Star Spectroscopic Survey (GOSSS). II. Bright Southern Stars". The Astrophysical Journal Supplement Series. 211 (1): 84. arXiv: 1312.6222 . Bibcode:2014ApJS..211...10S. doi:10.1088/0067-0049/211/1/10. S2CID   118847528. 10.
  4. 1 2 3 Rauw, G.; Vreux, J.-M.; Stevens, I. R.; Gosset, E.; Sana, H.; Jamar, C.; Mason, K. O. (2002). "Phase-resolved X-ray and optical spectroscopy of the massive binary HD 93403". Astronomy and Astrophysics. 388 (2): 552. Bibcode:2002A&A...388..552R. doi: 10.1051/0004-6361:20020523 .
  5. 1 2 3 Rauw, G.; Sana, H.; Gosset, E.; Vreux, J.-M.; Jehin, E.; Parmentier, G. (2000). "A new orbital solution for the massive binary system HD 93403". Astronomy and Astrophysics. 360: 1003. Bibcode:2000A&A...360.1003R.
  6. Analysis of the X-ray emission of OB stars: O stars
  7. Palate, M.; Rauw, G.; Koenigsberger, G.; Moreno, E. (2013). "Spectral modelling of massive binary systems". Astronomy & Astrophysics. 552: A39. arXiv: 1302.5201 . Bibcode:2013A&A...552A..39P. doi:10.1051/0004-6361/201219754. S2CID   54771449.