Astronomy:MWC 137

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Short description: Star in the constellation Canis Major
MWC 137
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A light curve for MWC 137, plotted from TESS data[1]
Observation data
Equinox J2000.0]] (ICRS)
Constellation Orion[2]
Right ascension  06h 18m 45.522s[3]
Declination +15° 16′ 52.24″[3]
Apparent magnitude (V) 11.47 to 11.62[4]
Characteristics
Evolutionary stage Supergiant[5]
Spectral type sgB[e][6]
B−V color index 1.700±0.495[2]
Variable type pulsating[5]
Astrometry
Radial velocity (Rv)+652.92±0.02[7] km/s
Proper motion (μ) RA: −0.294[3] mas/yr
Dec.: −0.510[3] mas/yr
Parallax (π)0.194 ± 0.0256[3] mas
Distance17,000±4,600 ly
(5,200±1,400 pc)
Absolute magnitude (MV)−7.2[6]
Details
Mass37+9
−5 M☉[8]
30 to 70[5] M☉
Radius26+29
−9[8] R☉
Luminosity690,000[5] L☉
Temperature28,200[5] K
Rotational velocity (v sin i)95.3[7] km/s
Age4.7±0.7[8] Myr
Other designations
V1308 Ori, HIP 29988, IRAS 06158+1517, 2MASS J06184553+1516522[9]
Database references
SIMBADdata

MWC 137 is a supergiant star in the equatorial constellation of Orion. It has the variable star designation V1308 Ori; MWC 137 is from the Mount Wilson Catalogue published in 1933.[10] The star is located at a distance of about 17.0 ± 4.6 thousand light-years (5.2 ± 1.4 kpc)*,[6] at the center of the filamentary nebula Sh 2-266.

Properties

This is a massive B[e] star that displays radial pulsational variabilities with a dominant period of around 1.9 days.[5] Evolutionary models show it to be near or in its post main sequence stage.[11] The star displays a jet – a large, collaminated outflow, which suggests the presence of an accretion disk.[6] An X-ray source detected by the SWIFT observatory may be associated with MWC 137, which suggests the presence of a neutron star companion.[12]

MWC 137 has a stellar classification of sgB[e],[6] where 'sg' indicates it is a supergiant-type B[e] star. The mass is uncertain, but lies in the range of 30 to 70 times the mass of the Sun.[5] In 2021, M. Kraus and associates found a mass estimate of roughy 37 solar masses.[8] It is radiating 690,000 times the luminosity of the Sun from its photosphere at an effective temperature of 28,200 K.[5]

This star is located at the center of the filamentary nebula Sh 2-266, which is elliptical in shape and spans an angular size of 80′ × 56′.[13] This has the form of a ring nebula, possibly as the result of stellar winds interacting with the interstellar medium or ejected matter.[14] A bow-shaped feature was discovered in 2021, at a position angle of 225°–245° at an angular separation of 80″ from MWC 137.[8] The star is directly associated with an H II region that spans an angular size of one arcminute.[15]

References

  1. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html. 
  2. ↑ 2.0 2.1 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A.  XHIP record for this object at VizieR.
  3. ↑ 3.0 3.1 3.2 3.3 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940.  Gaia DR3 record for this source at VizieR.
  4. ↑ Samus', N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (2017). "General catalogue of variable stars: Version GCVS 5.1". Astronomy Reports 61 (1): 80. doi:10.1134/S1063772917010085. Bibcode: 2017ARep...61...80S. 
  5. ↑ 5.0 5.1 5.2 5.3 5.4 5.5 5.6 5.7 Parida, Sugyan et al. (June 2024), "Instabilities in Models of Supergiants MWC 137 and MWC 314", Proceedings of the 3rd BINA Workshop on the Scientific Potential of the Indo-Belgian Cooperation, Bulletin de la Société Royale des Sciences de Liège, 93, pp. 552–559, doi:10.25518/0037-9565.11790, Bibcode: 2024BSRSL..93..552P. 
  6. ↑ 6.0 6.1 6.2 6.3 6.4 Mehner, A. et al. (January 2016), "VLT/MUSE discovers a jet from the evolved B[e] star MWC 137", Astronomy & Astrophysics 585: id. A81, doi:10.1051/0004-6361/201527180, Bibcode: 2016A&A...585A..81M. 
  7. ↑ 7.0 7.1 Jönsson, Henrik et al. (2020). "APOGEE Data and Spectral Analysis from SDSS Data Release 16: Seven Years of Observations Including First Results from APOGEE-South". The Astronomical Journal 160 (3): 120. doi:10.3847/1538-3881/aba592. Bibcode: 2020AJ....160..120J. 
  8. ↑ 8.0 8.1 8.2 8.3 8.4 Kraus, Michaela et al. (October 2021), "Resolving the Circumstellar Environment of the Galactic B[e] Supergiant Star MWC 137.II. Nebular Kinematics and Stellar Variability", The Astronomical Journal 162 (4): id. 150, doi:10.3847/1538-3881/ac1355, Bibcode: 2021AJ....162..150K. 
  9. ↑ "MWC 137". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=MWC+137. 
  10. ↑ "Catalogue and Bibliography of Stars of Classes B and A whose Spectra have Bright Hydrogen Lines", Astrophysical Journal 78: 87, September 1933, doi:10.1086/143490, Bibcode: 1933ApJ....78...87M. 
  11. ↑ Parida, Sugyan et al. (January 2024), "On the stability and pulsation in models of B[e] star MWC 137", Monthly Notices of the Royal Astronomical Society 527 (3): 7414–7423, doi:10.1093/mnras/stad3626, Bibcode: 2024MNRAS.527.7414P. 
  12. ↑ Mehner, A. et al. (February 2017), "The Jet from MWC 137 Points at a Supergiant B[e] Star in a Binary", in Miroshnichenko, Anatoly; Zharikov, Sergey; Korčáková, Daniela et al., The B[e] Phenomenon: Forty Years of Studies. Proceedings of a Conference held at Charles University, Prague, Czech Republic 27 June – 1 July 2016, ASP Conference Series, 508, San Francisco: Astronomical Society of the Pacific, p. 267, Bibcode: 2017ASPC..508..267M. 
  13. ↑ Ciatti, F.; Mammano, A. (February 1975), "Ejection of nebulae by BQ radiostars with infrared excess", Astronomy and Astrophysics 38: 435, Bibcode: 1975A&A....38..435C. 
  14. ↑ Esteban, Cesar; Fernandez, Matilde (July 1998), "S266: a ring nebula around a Galactic B[e] supergiant?", Monthly Notices of the Royal Astronomical Society 298 (1): 185–192, doi:10.1046/j.1365-8711.1998.01610.x, Bibcode: 1998MNRAS.298..185E. 
  15. ↑ Fuente, A. et al. (November 2003), "First Evidence of Dusty Disks around Herbig Be Stars", The Astrophysical Journal 598 (1): L39–L42, doi:10.1086/380296, Bibcode: 2003ApJ...598L..39F. 

Further reading

  • Kraus, Michaela et al. (November 2017), "Resolving the Circumstellar Environment of the Galactic B[e] Supergiant Star MWC 137 from Large to Small Scales", The Astronomical Journal 154 (5): id. 186, doi:10.3847/1538-3881/aa8df6, Bibcode: 2017AJ....154..186K. 
  • Alimardanova, F. et al. (February 2017), "Spectroscopy and Photometry of MWC 137", in Miroshnichenko, Anatoly; Zharikov, Sergey; Korčáková, Daniela et al., The B[e] Phenomenon: Forty Years of Studies. Proceedings of a Conference held at Charles University, Prague, Czech Republic 27 June – 1 July 2016, ASP Conference Series, 508, San Francisco: Astronomical Society of the Pacific, p. 355, Bibcode: 2017ASPC..508..355A. 
  • Kraus, M. et al. (February 2017), "Clumpy Molecular Structures Revolving the B[e] Supergiant MWC 137", in Miroshnichenko, Anatoly; Zharikov, Sergey; Korčáková, Daniela et al., The B[e] Phenomenon: Forty Years of Studies. Proceedings of a Conference held at Charles University, Prague, Czech Republic 27 June – 1 July 2016, ASP Conference Series, 508, San Francisco: Astronomical Society of the Pacific, p. 381, Bibcode: 2017ASPC..508..381K. 
  • Muratore, M. F. et al. (January 2015), "Evidence of the Evolved Nature of the B[e] Star MWC 137", The Astronomical Journal 149 (1): id. 13, doi:10.1088/0004-6256/149/1/13, Bibcode: 2015AJ....149...13M. 
  • Kondratyeva, L. N. (2007), "The Object MWC 137", Odessa Astronomical Publications 20: 86, Bibcode: 2007OAP....20...86K. 



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