HD 64568

Last updated

HD 64568
Puppis IAU.svg
Red circle.svg
Location of HD 64568 (circled)
Observation data
Epoch J2000.0 [1]        Equinox J2000.0 [1]
Constellation Puppis
Right ascension 07h 53m 38.20519s
Declination −26° 14′ 02.5981″
Apparent magnitude  (V)9.39 [2]
Characteristics
Evolutionary stage Main-sequence star
Spectral type O3V((f*))z [3]
U−B color index −0.86 [2]
B−V color index 0.11 [2]
J−H color index 0.001 [4]
J−K color index 0.008 [4]
Astrometry
Radial velocity (Rv)87.1±5.7 [5]  km/s
Proper motion (μ)RA: −0.535 [1]   mas/yr
Dec.: 4.115 [1]   mas/yr
Parallax (π)0.2241 ± 0.0177  mas [1]
Distance 15,000 ± 1,000  ly
(4,500 ± 400  pc)
Details [5]
Mass 57 [6]   M☉
Radius 14±2 [6]   R☉
Luminosity 500000+290000
−180000 [6]   L☉
Surface gravity (log g)3.91±0.08  cgs
Temperature 44900±1700  K
Rotational velocity (v sin i)≤117±13 km/s
Other designations
CD−25° 5228, CPD−25° 3039, Gaia DR2  5602033390154015744, HD  64568, HIP  38548, SAO  174748, PPM  253404, TIC  128808726, TYC  6557-214-1, GSC  06557-00214, 2MASS J07533820-2614025, DENIS J075338.2-261402, NGC 2467 77 [7]
Database references
SIMBAD data

HD 64568 is a massive solitary [8] star in the southern constellation of Puppis. With an apparent magnitude of 9.39, it is too faint to be seen by the naked eye, but can barely be observed by binoculars, appearing as a blue-hued dot of light. It is located approximately 4,500 parsecs (15,000 light-years) distant according to Gaia EDR3 parallax measurements.

Properties

NGC 2467 and Surroundings.jpg
Red circle.svg
HD 64568
Image of NGC 2467 from ESO. HD 64568 (circled) is in the top right.

HD 64568 belongs to an OB association named Puppis OB2, which is part of the star-forming region NGC 2467. It is one of the ionizing stars of the H II region Sh 2-311. [6]

This is a very early O-type main-sequence star that is among the most massive stars, weighing 57 times the mass of the Sun, but has a comparatively modest radius of 14 R☉. It radiates roughly 500,000 times the luminosity of the Sun from its photosphere at an effective temperature of 44,900 K (44,600 °C; 80,400 °F). It is losing mass to stellar winds, but the rate at which this occurs is highly uncertain, with two models yielding values of 5.6±5.0×10−7M☉/yr and 2.3×10−6M☉/yr. [6]

In 1982, it was given the spectral type O3V((f*)), becoming the first object of its kind. The ((f*)) suffix signifies the presence of weak N IV (N3+) 4058 Å emission line and N V (N4+) absorption lines, the lack of any N III (N2+) emission, along with the strong He II (He+) 4686 Å absorption. [9] Radial velocity variations were discovered in 1986, which, at the time, was theorized to be either caused by an unseen binary companion or atmospheric instabilities seen in massive stars. [10] The latter theory was confirmed to be true by Markova (2011) as there was no evidence for a secondary object, and the variations are now thought to be the result of stellar pulsations and/or stellar wind variations. The same study also corroborated the O3V((f*)) classification. [8] Sota et al. (2014) updated the spectral type to O3V((f*))z, with the added "z" suffix to indicate that the 4686 Å helium line is abnormally strong. [3]

Related Research Articles

<span class="mw-page-title-main">Naos (star)</span> Star in the constellation of Puppis

Naos, also known by its Bayer designation of Zeta Puppis, is the brightest star in the constellation of Puppis.

<span class="mw-page-title-main">Mu Columbae</span> Star in the constellation Columba

Mu Columbae is a star in the constellation of Columba. It is one of the few O-class stars that are visible to the unaided eye. The star is known to lie approximately 1,900 light years from the Solar System.

<span class="mw-page-title-main">HD 95109</span> Star in the constellation Carina

HD 95109 is a Classical Cepheid variable, a type of variable star, in the constellation Carina. Its apparent magnitude is 6.86.

<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">RS Puppis</span> Variable star in the constellation Puppis

RS Puppis is a Cepheid variable star around 6,000 ly away in the constellation of Puppis. It is one of the biggest and brightest known Cepheids in the Milky Way galaxy and has one of the longest periods for this class of star at 41.5 days.

<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">HD 269810</span> Star in the constellation Dorado

HD 269810 is a blue giant star in the Large Magellanic Cloud. It is one of the most massive and most luminous stars known, and one of only a handful of stars with the spectral type O2. The star's name, HD 269810, comes from the Henry Draper Catalogue. The serial number 269810 indicates it was published in the extension of the catalogue and is formally referred to as HDE 269810.

<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">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 of 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.

Theta<sup>2</sup> Orionis Star in the constellation Orion

Theta2 Orionis is a multiple star system in the constellation Orion. It is a few arc minutes from its more famous neighbour the Trapezium Cluster, also known as θ1 Orionis.

<span class="mw-page-title-main">V3903 Sagittarii</span> Binary star system in the constellation Sagittarius

V3903 Sagittarii is an eclipsing binary star system in the constellation Sagittiarus. It creates an H II region LBN 29 1,070 parsecs away from the Sun.

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.

<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 the 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 1</span> Star in the constellation Cassiopeia

WR 1 is a Wolf-Rayet star located around 10,300 light years away from Earth in the constellation of Cassiopeia. It is only slightly more than twice the size of the sun, but due to a temperature over 100,000 K it is over 758,000 times as luminous as the sun.

WR 3 is a Wolf-Rayet star located around 9,500 light years away from Earth in the constellation of Cassiopeia.

<span class="mw-page-title-main">NGC 7419</span> Open cluster in the constellation Cepheus

NGC 7419 is an open cluster in the constellation Cepheus. It is heavily reddened and notable for containing five red supergiants, the highest number known in any cluster until the end of the 20th century, but probably no blue supergiants.

<span class="mw-page-title-main">HD 73882</span> Eclipsing binary system in constellation Vela

HD 73882 is a visual binary system with the components separated by 0.6″ and a combined spectral class of O8. One of stars is an eclipsing binary system. The period of variability is listed as both 2.9199 days and 20.6 days, possibly due to the secondary being a spectroscopic binary star.

<span class="mw-page-title-main">NGC 1624-2</span> Star in the constellation Perseus

NGC 1624-2 is a massive O-type star located in the star cluster NGC 1624, in the constellation of Perseus, about 16,800 light years away. NGC 1624-2 is notable for being most strongly magnetised O-type star known, with a magnetic field strength of 20 kG, or about 20,000 times the Sun's magnetic field strength. It hosts a large and dense magnetosphere, formed from the interaction between its very strong magnetic field and its dense, radiatively-driven stellar wind, which also absorbs up to 95% of x-rays generated from around the star.

References

  1. 1 2 3 4 5 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics . 649: A1. arXiv: 2012.01533 . Bibcode:2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657 . S2CID   227254300. (Erratum:  doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  2. 1 2 3 Lodén, L. O. (1966). "A study of NGC 2467 an dthe association Pup I". Arkiv för Astronomii. 4: 65-72. Bibcode:1966ArA.....4...65L.
  3. 1 2 Sota, A.; Apellániz, J. Maíz; Morrell, N. I.; Barbá, R. H.; Walborn, N. R.; Gamen, R. C.; Arias, J. I.; Alfaro, E. J. (25 February 2014). "The Galactic O-Star Spectroscopic Survey (Gosss). Ii. Bright Southern Stars". The Astrophysical Journal Supplement Series. 211 (1): 10. arXiv: 1312.6222 . Bibcode:2014ApJS..211...10S. doi: 10.1088/0067-0049/211/1/10 . ISSN   0067-0049.
  4. 1 2 Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E.; Fowler, John W.; Gizis, John E.; Howard, Elizabeth V.; Huchra, John P.; Jarrett, Thomas H.; Kopan, Eugene L.; Kirkpatrick, J. Davy; Light, Robert M.; Marsh, Kenneth A.; McCallon, Howard L.; Schneider, Stephen E.; Stiening, Rae; Sykes, Matthew J.; Weinberg, Martin D.; Wheaton, William A.; Wheelock, Sherry L.; Zacarias, N. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues. 2246: II/246. Bibcode:2003yCat.2246....0C.
  5. 1 2 Williams, S. J.; Gies, D. R.; Hillwig, T. C.; McSwain, M. V.; Huang, W. (1 November 2011). "Radial Velocities of Galactic O-Type Stars. I. Short-Term Constant Velocity Stars". The Astronomical Journal. 142 (5): 146. Bibcode:2011AJ....142..146W. doi: 10.1088/0004-6256/142/5/146 . ISSN   0004-6256.
  6. 1 2 3 4 5 Garcia, Miriam; Bianchi, Luciana (2004). "The Effective Temperatures of Hot Stars. II. The Early-O Types". The Astrophysical Journal. 606 (1): 497–513. arXiv: astro-ph/0402207 . Bibcode:2004ApJ...606..497G. doi: 10.1086/383002 . ISSN   0004-637X.
  7. ↑ "HD 64568". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 6 December 2024.
  8. 1 2 Markova, N.; Puls, J.; Scuderi, S.; Simón-Díaz, S.; Herrero, A. (2011). "Spectroscopic and physical parameters of Galactic O-type stars: I. Effects of rotation and spectral resolving power in the spectral classification of dwarfs and giants". Astronomy & Astrophysics. 530: A11. arXiv: 1103.3357 . Bibcode:2011A&A...530A..11M. doi: 10.1051/0004-6361/201015956 . ISSN   0004-6361.
  9. ↑ Walborn, N. R. (1982). "The O3 stars". The Astrophysical Journal. 254: L15. Bibcode:1982ApJ...254L..15W. doi: 10.1086/183747 . ISSN   0004-637X.
  10. ↑ Solivella, G. R.; Niemela, V. S. (February 1986). "A radial velocity study of two early O stars". Revista Mexicana de Astronomia y Astrofisica. 12: 188. Bibcode:1986RMxAA..12..188S.
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.