WR 46

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WR 46
Crux.jpg
Cercle vert 100%.svg
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) 0.47 ± 0.33[6] mas
Distance 4,070[7] pc
Absolute magnitude (MV) −3.50[3]
Details
Mass 25[3] M
Radius 2.11[3] R
Luminosity 630,000[3] L
Temperature 112,000[3] K
Other designations
HD 104994, HIP 58954, DI Crucis, CD-613331, GSC 08978-02316, 2MASS J12051871-6203101, AAVSO 1200-61
Database references
SIMBAD data

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[edit]

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.[8] 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[edit]

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.[9] Theories that are now discounted include WR 46 being a Super soft X-ray source[10] or a V Sagittae star,[11]

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[12] Non-radial pulsations have been proposed, with multiple pulsation periods of varying amplitude accounting for the apparently irregular brightness changes.[4]

Binary star[edit]

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[10] and 0.329 days.[13] Most recent research refutes the idea of a companion, instead favoring the single WN star theory.[14]

References[edit]

  1. ^ a b c d Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653. arXiv:0708.1752Freely accessible. 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. Bibcode:2003AJ....125.2531R. doi:10.1086/374771. ISSN 0004-6256. 
  3. ^ a b c d e f Hamann, W. -R.; Gräfener, G.; Liermann, A. (2006). "The Galactic WN stars". Astronomy and Astrophysics. 457 (3): 1015. arXiv:astro-ph/0608078Freely accessible. Bibcode:2006A&A...457.1015H. doi:10.1051/0004-6361:20065052. 
  4. ^ a b c 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. arXiv:1104.4497Freely accessible. Bibcode:2011ApJ...735...13H. 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. arXiv:astro-ph/0406573Freely accessible. Bibcode:2004A&A...424..727P. doi:10.1051/0004-6361:20041213. ISSN 0004-6361. 
  6. ^ Gaia Collaboration (2016). "VizieR Online Data Catalog: Gaia DR1 (Gaia Collaboration, 2016)". VizieR On-line Data Catalog: I/337. Originally published in: Astron. Astrophys. 1337. Bibcode:2016yCat.1337....0G. 
  7. ^ Van Der Hucht, K. A. (2001). "The VIIth catalogue of galactic Wolf–Rayet stars". New Astronomy Reviews. 45 (3): 135. Bibcode:2001NewAR..45..135V. doi:10.1016/S1387-6473(00)00112-3. 
  8. ^ Pollock, A. M. T. (1987). "The Einstein view of the Wolf-Rayet stars". The Astrophysical Journal. 320: 283. Bibcode:1987ApJ...320..283P. doi:10.1086/165539. 
  9. ^ Zhekov, S. A. (2012). "X-rays from colliding stellar winds: The case of close Wolf-Rayet+O binary systems". Monthly Notices of the Royal Astronomical Society. 422 (2): 1332. arXiv:1202.1386Freely accessible. Bibcode:2012MNRAS.422.1332Z. doi:10.1111/j.1365-2966.2012.20706.x. 
  10. ^ a b Bibcode1995IAUS..163..245N
  11. ^ Steiner, J. E.; Diaz, M. P. (1998). "The V Sagittae Stars". Publications of the Astronomical Society of the Pacific. 110 (745): 276. Bibcode:1998PASP..110..276S. doi:10.1086/316139. 
  12. ^ 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. Bibcode:2000AJ....120.2101M. doi:10.1086/301580. ISSN 0004-6256. 
  13. ^ 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. Bibcode:2000AJ....120.2101M. doi:10.1086/301580. 
  14. ^ Gosset, E.; De Becker, M.; Nazé, Y.; Carpano, S.; Rauw, G.; Antokhin, I. I.; Vreux, J. -M.; Pollock, A. M. T. (2011). "XMM-Newtonobservation of the enigmatic object WR 46". Astronomy & Astrophysics. 527: A66. Bibcode:2011A&A...527A..66G. doi:10.1051/0004-6361/200912510.