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m Bot: Deprecating Template:Cite doi and some minor fixes
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|dist_pc = 4,070<ref name=hucht>{{cite doi|10.1016/S1387-6473(00)00112-3}}</ref>
|dist_pc = 4,070<ref name=hucht>{{Cite journal | doi = 10.1016/S1387-6473(00)00112-3| title = The VIIth catalogue of galactic Wolf–Rayet stars| year = 2001| last1 = Van Der Hucht | first1 = K. A. | journal = New Astronomy Reviews| volume = 45| issue = 3| pages = 135}}</ref>
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==Features==
==Features==
WR 46 has [[spectral type]] WN3, with peculiarities in the spectrum including unusually broad [[Spectral line|emission lines]]. Its [[Electromagnetic spectrum|spectrum]] is characterized by the presence of strong lines of N<sub>V</sub> and He<sub>II</sub> and the absence of [[hydrogen]] lines. It is known as a weak-lined WNE star because of the high temperature but relatively weak emission strength.<ref name=henault>{{cite doi|10.1088/0004-637X/735/1/13}}</ref>
WR 46 has [[spectral type]] WN3, with peculiarities in the spectrum including unusually broad [[Spectral line|emission lines]]. Its [[Electromagnetic spectrum|spectrum]] is characterized by the presence of strong lines of N<sub>V</sub> and He<sub>II</sub> and the absence of [[hydrogen]] lines. It is known as a weak-lined WNE star because of the high temperature but relatively weak emission strength.<ref name=henault>{{Cite journal | doi = 10.1088/0004-637X/735/1/13| title = New Constraints on the Origin of the Short-Term Cyclical Variability of the Wolf-Rayet Star Wr 46| journal = The Astrophysical Journal| volume = 735| pages = 13| year = 2011| last1 = Hénault-Brunet | first1 = V.| last2 = St-Louis | first2 = N.| last3 = Marchenko | first3 = S. V.| last4 = Pollock | first4 = A. M. T.| last5 = Carpano | first5 = S.| last6 = Talavera | first6 = A.}}</ref>


The physical parameters of WR 46 are all estimates from assumptions about the distance and models for stars of its type, complicated by the suspicion that there is a companion star. The [[effective temperature]] is over 110,000K, the luminosity greater than 600,000 times the [[solar luminosity]] ({{Solar luminosity|link=y}}), the mass around 25 times that of the [[Sun]] ({{Solar mass|link=y}}) and a radius of 2.9 times the [[solar radius]] ({{Solar radius|link=y}}). The [[terminal velocity]] of the [[stellar wind]] reaches 2450&nbsp;km/s with a total mass loss rate of 4 × 10<sup>−6</sup> {{Solar mass}} per [[year]].
The physical parameters of WR 46 are all estimates from assumptions about the distance and models for stars of its type, complicated by the suspicion that there is a companion star. The [[effective temperature]] is over 110,000K, the luminosity greater than 600,000 times the [[solar luminosity]] ({{Solar luminosity|link=y}}), the mass around 25 times that of the [[Sun]] ({{Solar mass|link=y}}) and a radius of 2.9 times the [[solar radius]] ({{Solar radius|link=y}}). The [[terminal velocity]] of the [[stellar wind]] reaches 2450&nbsp;km/s with a total mass loss rate of 4 × 10<sup>−6</sup> {{Solar mass}} per [[year]].


WR 46 is a known source of X-rays, an aspect that was discovered by the Einstein Observatory.<ref name=pollock>{{cite doi|10.1086/165539}}</ref> The X-ray [[luminosity]] between 0.2 and 10.0 keV is 7.7 × 10<sup>32</sup> erg/s. Its X-ray spectrum is dominated by a soft component but there is also a hard component above 3 keV (a hard tail).
WR 46 is a known source of X-rays, an aspect that was discovered by the Einstein Observatory.<ref name=pollock>{{Cite journal | doi = 10.1086/165539| title = The Einstein view of the Wolf-Rayet stars| journal = The Astrophysical Journal| volume = 320| pages = 283| year = 1987| last1 = Pollock | first1 = A. M. T.}}</ref> The X-ray [[luminosity]] between 0.2 and 10.0 keV is 7.7 × 10<sup>32</sup> erg/s. Its X-ray spectrum is dominated by a soft component but there is also a hard component above 3 keV (a hard tail).


==Variability==
==Variability==
WR 46 exhibits complex variability on relatively short time scales of a few hours. In the past there have been regular but intermittent changes in the [[radial velocity]], multiple periods and [[Photometry (astronomy)|photometric]] variation at some wavelengths, particularly [[ultraviolet]]. It has been proposed that this short-term behavior is due to non-radial pulsations, fast rotational modulation, or the presence of a lower-mass companion.<ref name=zhekov>{{cite doi|10.1111/j.1365-2966.2012.20706.x}}</ref> Theories that are now discounted include WR 46 being a [[Super soft X-ray source]]<ref name=niemela/> or a V Sagittae star,<ref name=steiner>{{cite doi|10.1086/316139}}</ref>
WR 46 exhibits complex variability on relatively short time scales of a few hours. In the past there have been regular but intermittent changes in the [[radial velocity]], multiple periods and [[Photometry (astronomy)|photometric]] variation at some wavelengths, particularly [[ultraviolet]]. It has been proposed that this short-term behavior is due to non-radial pulsations, fast rotational modulation, or the presence of a lower-mass companion.<ref name=zhekov>{{cite doi|10.1111/j.1365-2966.2012.20706.x}}</ref> Theories that are now discounted include WR 46 being a [[Super soft X-ray source]]<ref name=niemela/> or a V Sagittae star,<ref name=steiner>{{Cite journal | doi = 10.1086/316139| title = The V Sagittae Stars| journal = Publications of the Astronomical Society of the Pacific| volume = 110| issue = 745| pages = 276| year = 1998| last1 = Steiner | first1 = J.  E. | last2 = Diaz | first2 = M.  P. }}</ref>


The radial velocity changes of the spectral lines originating most deeply within the [[stellar wind]] show clear radial velocity variations with a period of 7.9 hours. However the lines do not change their shape or intensity, which would be expected from a pulsating star<ref name="marchenko2000>{{cite journal|last1=Marchenko|first1=Sergey V.|last2=Arias|first2=Julia|last3=Barbá|first3=Rodolfo|last4=Balona|first4=Luis|last5=Moffat|first5=Anthony F. J.|last6=Niemela|first6=Virpi S.|last7=Shara|first7=Michael M.|last8=Sterken|first8=Christiaan|title=The Puzzle of HD 104994 (WR 46)|journal=The Astronomical Journal|volume=120|issue=4|year=2000|pages=2101–2113|issn=00046256|doi=10.1086/301580}}</ref>
The radial velocity changes of the spectral lines originating most deeply within the [[stellar wind]] show clear radial velocity variations with a period of 7.9 hours. However the lines do not change their shape or intensity, which would be expected from a pulsating star<ref name="marchenko2000>{{cite journal|last1=Marchenko|first1=Sergey V.|last2=Arias|first2=Julia|last3=Barbá|first3=Rodolfo|last4=Balona|first4=Luis|last5=Moffat|first5=Anthony F. J.|last6=Niemela|first6=Virpi S.|last7=Shara|first7=Michael M.|last8=Sterken|first8=Christiaan|title=The Puzzle of HD 104994 (WR 46)|journal=The Astronomical Journal|volume=120|issue=4|year=2000|pages=2101–2113|issn=00046256|doi=10.1086/301580}}</ref>


==Binary star==
==Binary star==
WR 46 has been suspected to be a [[Binary star|binary system]] with an OB companion. The [[orbital period]] of the system has been reported at 0.311 days<ref name=niemela>{{bibcode|1995IAUS..163..245N}}</ref> and 0.329 days.<ref name=marchenko>{{cite doi|10.1086/301580}}</ref> Most recent research refutes the idea of a companion, instead favoring the single WN star theory.<ref name=gosset>{{cite doi|10.1051/0004-6361/200912510
WR 46 has been suspected to be a [[Binary star|binary system]] with an OB companion. The [[orbital period]] of the system has been reported at 0.311 days<ref name=niemela>{{bibcode|1995IAUS..163..245N}}</ref> and 0.329 days.<ref name=marchenko>{{Cite journal | doi = 10.1086/301580| title = The Puzzle of HD 104994 (WR 46)| journal = The Astronomical Journal| volume = 120| issue = 4| pages = 2101| year = 2000| last1 = Marchenko | first1 = S. V. | last2 = Arias | first2 = J. | last3 = Barbá | first3 = R. | last4 = Balona | first4 = L. | last5 = Moffat | first5 = A. F. J. | last6 = Niemela | first6 = V. S. | last7 = Shara | first7 = M. M. | last8 = Sterken | first8 = C. }}</ref> Most recent research refutes the idea of a companion, instead favoring the single WN star theory.<ref name=gosset>{{cite doi|10.1051/0004-6361/200912510
}}</ref>
}}</ref>


Revision as of 17:33, 29 August 2015

WR 46
WR 46 (location circled) in the constellation Crux
Observation data
Epoch J2000      Equinox J2000
Constellation Crux
Right ascension 12h 05m 18.72028s[1]
Declination −62° 03′ 10.1280″[1]
Apparent magnitude (V) 10.83[2]
Characteristics
Spectral type WN3p-w[3]
U−B color index -0.84[2]
B−V color index -0.03[2]
Variable type Irregular[4]
Astrometry
Radial velocity (Rv)4.00[5] km/s
Proper motion (μ) RA: -5.44[1] mas/yr
Dec.: 1.84[1] mas/yr
Parallax (π)2.45 mas[1]
Distance4,070[6] pc
Absolute magnitude (MV)−3.50[3]
Details
Mass25[3] M☉
Radius2.11[3] R☉
Luminosity630,000[3] L☉
Temperature112,000[3] K
Other designations
HD 104994, HIP 58954, DI Crucis, CD-613331, GSC 08978-02316, 2MASS J12051871-6203101, AAVSO 1200-61
Database references
SIMBADdata

WR 46 (DI Crucis) 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 OB4 Cru, and is around 4,000 parsecs or 13,000 light years from the Solar System.

Features

WR 46 has spectral type WN3, with peculiarities in the spectrum including unusually broad emission lines. Its spectrum is characterized by the presence of strong lines of NV and HeII and the absence of hydrogen lines. It is known as a weak-lined WNE star because of the high temperature but relatively weak emission strength.[4]

The physical parameters of WR 46 are all estimates from assumptions about the distance and models for stars of its type, complicated by the suspicion that there is a companion star. The effective temperature is over 110,000K, the luminosity greater than 600,000 times the solar luminosity (L☉), the mass around 25 times that of the Sun (M☉) and a radius of 2.9 times the solar radius (R☉). The terminal velocity of the stellar wind reaches 2450 km/s with a total mass loss rate of 4 × 10−6 M☉ per year.

WR 46 is a known source of X-rays, an aspect that was discovered by the Einstein Observatory.[7] The X-ray luminosity between 0.2 and 10.0 keV is 7.7 × 1032 erg/s. Its X-ray spectrum is dominated by a soft component but there is also a hard component above 3 keV (a hard tail).

Variability

WR 46 exhibits complex variability on relatively short time scales of a few hours. In the past there have been regular but intermittent changes in the radial velocity, multiple periods and photometric variation at some wavelengths, particularly ultraviolet. It has been proposed that this short-term behavior is due to non-radial pulsations, fast rotational modulation, or the presence of a lower-mass companion.[8] Theories that are now discounted include WR 46 being a Super soft X-ray source[9] or a V Sagittae star,[10]

The radial velocity changes of the spectral lines originating most deeply within the stellar wind show clear radial velocity variations with a period of 7.9 hours. However the lines do not change their shape or intensity, which would be expected from a pulsating star[11]

Binary star

WR 46 has been suspected to be a binary system with an OB companion. The orbital period of the system has been reported at 0.311 days[9] and 0.329 days.[12] Most recent research refutes the idea of a companion, instead favoring the single WN star theory.[13]

References

  1. ^ a b c d e Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357.
  2. ^ a b c Reed, B. Cameron (2003). "Catalog of Galactic OB Stars". The Astronomical Journal. 125 (5): 2531–2533. doi:10.1086/374771. ISSN 0004-6256.
  3. ^ a b c d e f Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1051/0004-6361:20065052, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1051/0004-6361:20065052 instead.
  4. ^ a b Hénault-Brunet, V.; St-Louis, N.; Marchenko, S. V.; Pollock, A. M. T.; Carpano, S.; Talavera, A. (2011). "New Constraints on the Origin of the Short-Term Cyclical Variability of the Wolf-Rayet Star Wr 46". The Astrophysical Journal. 735: 13. doi:10.1088/0004-637X/735/1/13.
  5. ^ Pourbaix, D.; Tokovinin, A. A.; Batten, A. H.; Fekel, F. C.; Hartkopf, W. I.; Levato, H.; Morrell, N. I.; Torres, G.; Udry, S. (2004). "SB9: The ninth catalogue of spectroscopic binary orbits". Astronomy and Astrophysics. 424 (2): 727–732. doi:10.1051/0004-6361:20041213. ISSN 0004-6361.
  6. ^ Van Der Hucht, K. A. (2001). "The VIIth catalogue of galactic Wolf–Rayet stars". New Astronomy Reviews. 45 (3): 135. doi:10.1016/S1387-6473(00)00112-3.
  7. ^ Pollock, A. M. T. (1987). "The Einstein view of the Wolf-Rayet stars". The Astrophysical Journal. 320: 283. doi:10.1086/165539.
  8. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1111/j.1365-2966.2012.20706.x, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1111/j.1365-2966.2012.20706.x instead.
  9. ^ a b Bibcode:1995IAUS..163..245N
  10. ^ Steiner, J.  E.; Diaz, M.  P. (1998). "The V Sagittae Stars". Publications of the Astronomical Society of the Pacific. 110 (745): 276. doi:10.1086/316139. {{cite journal}}: no-break space character in |first1= at position 4 (help); no-break space character in |first2= at position 4 (help)
  11. ^ Marchenko, Sergey V.; Arias, Julia; Barbá, Rodolfo; Balona, Luis; Moffat, Anthony F. J.; Niemela, Virpi S.; Shara, Michael M.; Sterken, Christiaan (2000). "The Puzzle of HD 104994 (WR 46)". The Astronomical Journal. 120 (4): 2101–2113. doi:10.1086/301580. ISSN 0004-6256.
  12. ^ Marchenko, S. V.; Arias, J.; Barbá, R.; Balona, L.; Moffat, A. F. J.; Niemela, V. S.; Shara, M. M.; Sterken, C. (2000). "The Puzzle of HD 104994 (WR 46)". The Astronomical Journal. 120 (4): 2101. doi:10.1086/301580.
  13. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1051/0004-6361/200912510 , please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1051/0004-6361/200912510 instead.

This article is based on the Spanish version es.wikipedia.org/wiki/DI Crucis

Retrieved from "https://en.wikipedia.org/w/index.php?title=WR_46&oldid=678484486"