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MWC 137

MWC 137

A light curve for MWC 137, plotted from TESS data[1]
Observation data
Epoch J2000      Equinox 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 mas/yr[3]
Dec.: −0.510 mas/yr[3]
Parallax (π)0.194±0.0256 mas[3]
Distance17,000±4,600 ly
(5,200±1,400 pc)[6]
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 roughly 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. Retrieved 19 October 2025.
  2. ^ a b Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015. XHIP record for this object at VizieR.
  3. ^ a b c d Vallenari, A.; et al. (Gaia collaboration) (2023), "Gaia Data Release 3. Summary of the content and survey properties", Astronomy and Astrophysics, 674: A1, arXiv:2208.00211, Bibcode:2023A&A...674A...1G, doi:10.1051/0004-6361/202243940, S2CID 244398875. 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. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085.
  5. ^ a b c d e f g h 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, vol. 93, pp. 552–559, arXiv:2401.09046, Bibcode:2024BSRSL..93..552P, doi:10.25518/0037-9565.11790.
  6. ^ a b c d e f Mehner, A.; et al. (January 2016), "VLT/MUSE discovers a jet from the evolved B[e] star MWC 137", Astronomy & Astrophysics, 585, id. A81, arXiv:1511.02289, Bibcode:2016A&A...585A..81M, doi:10.1051/0004-6361/201527180.
  7. ^ a b 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. arXiv:2007.05537. Bibcode:2020AJ....160..120J. doi:10.3847/1538-3881/aba592.
  8. ^ a b c d e 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, arXiv:2106.15981, Bibcode:2021AJ....162..150K, doi:10.3847/1538-3881/ac1355.
  9. ^ "MWC 137", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2025-07-19.
  10. ^ Merrill, Paul W.; Burwell, Cora G. (September 1933), "Catalogue and Bibliography of Stars of Classes B and A whose Spectra have Bright Hydrogen Lines", Astrophysical Journal, 78: 87, Bibcode:1933ApJ....78...87M, doi:10.1086/143490.
  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, arXiv:2311.12549, Bibcode:2024MNRAS.527.7414P, doi:10.1093/mnras/stad3626.
  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; et al. (eds.), 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, vol. 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, Bibcode:1998MNRAS.298..185E, doi:10.1046/j.1365-8711.1998.01610.x.
  15. ^ Fuente, A.; et al. (November 2003), "First Evidence of Dusty Disks around Herbig Be Stars", The Astrophysical Journal, 598 (1): L39–L42, arXiv:astro-ph/0310062, Bibcode:2003ApJ...598L..39F, doi:10.1086/380296.

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, arXiv:1709.06439, Bibcode:2017AJ....154..186K, doi:10.3847/1538-3881/aa8df6.
  • Alimardanova, F.; et al. (February 2017), "Spectroscopy and Photometry of MWC 137", in Miroshnichenko, Anatoly; et al. (eds.), 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, vol. 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; et al. (eds.), 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, vol. 508, San Francisco: Astronomical Society of the Pacific, p. 381, arXiv:1610.05596, 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, arXiv:1409.7550, Bibcode:2015AJ....149...13M, doi:10.1088/0004-6256/149/1/13.
  • Kondratyeva, L. N. (2007), "The Object MWC 137", Odessa Astronomical Publications, 20: 86, Bibcode:2007OAP....20...86K.

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