Epsilon_Persei

Epsilon Persei

Epsilon Persei

Star system in the constellation Perseus

Epsilon Persei, Latinized from ε Persei, is a multiple star system in the northern constellation of Perseus. It has a combined apparent visual magnitude of +2.88,[2] which is bright enough to be viewed with the naked eye. Based upon parallax measurements, this system is located at a distance of roughly 640 light-years (196 parsecs) from Earth.[1]

Quick Facts Observation data Epoch J2000 Equinox J2000, Constellation ...

This is a spectroscopic binary system, which means that the presence of an orbiting companion has been revealed by radial velocity variations in the spectrum of the primary. The two components are orbiting each other with a period of 14 days at a high orbital eccentricity of 0.55. The secondary component has about 6–13% of the primary's mass and may have a stellar classification in the range from A6 V to K1 V. There may be a third component to this system with an orbital period of roughly 9,428 days (25.8 years), although this has not been conclusively demonstrated. If this component exists, it would have about 51–139% of the primary's mass. This high level of uncertainty is because the inclination of the orbit is not known.[5]

A light curve for Epsilon Persei, plotted from Hipparcos data[11]

The primary component of this system is a massive star with 12–16[5] times the Sun's mass and near eight times the radius of the Sun.[6] It was chosen as an MK spectral standard for the class B0.5III,[3] making it a giant star that has evolved away from the main sequence. It has also been classified as a main sequence star, reflecting its evolutionary state near or slightly beyind the end of core hydrogen fusion.[6] Component A is radiating over 28,000[7] times the Sun's luminosity from its outer envelope at an effective temperature of 26,500 K.[7] This gives the star the blue-white hue that is typical of B-type stars.[12] It is also a Beta Cephei variable star with a primary pulsation period of 0.1603 days, or 6.24 cycles per day. It may have multiple pulsation frequencies.[4]

Epsilon Persei has several resolved companions listed in multiple star catalogues: component B is a 9th-magnitude A2 main sequence star 9″ away and considered to be a common proper motion companion although they are too far apart for any orbital motion to be observed; component C is a 14th-magnitude background star about 80″ away; and HD 275984 163″ away is thought to be another common-proper-motion companion.[13][9]

References

  1. [1]
    van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600
  2. [2]
    Lutz, T. E.; Lutz, J. H. (June 1977), "Spectral classification and UBV photometry of bright visual double stars", Astronomical Journal, 82: 431–434, Bibcode:1977AJ.....82..431L, doi:10.1086/112066
  3. [3]
    Morgan, W. W.; Abt, Helmut A.; Tapscott, J. W. (1978), Revised MK Spectral Atlas for stars earlier than the sun, Bibcode:1978rmsa.book.....M
  4. [4]
    Stankov, Anamarija; Handler, Gerald (June 2005), "Catalog of Galactic β Cephei Stars", The Astrophysical Journal Supplement Series, 158 (2): 193–216, arXiv:astro-ph/0506495, Bibcode:2005ApJS..158..193S, doi:10.1086/429408, S2CID 119526948
  5. [5]
    Libich, J.; et al. (February 2006), "The new orbital elements and properties of ɛ Persei", Astronomy and Astrophysics, 446 (2): 583–589, Bibcode:2006A&A...446..583L, doi:10.1051/0004-6361:20053032, hdl:2066/35168. Results per solution 6.
  6. [6]
    Howe, K. S.; Clarke, C. J. (January 2009), "An analysis of v sin (i) correlations in early-type binaries", Monthly Notices of the Royal Astronomical Society, 392 (1): 448–454, Bibcode:2009MNRAS.392..448H, doi:10.1111/j.1365-2966.2008.14073.x
  7. [7]
    Hohle, M. M.; Neuhäuser, R.; Schutz, B. F. (April 2010), "Masses and luminosities of O- and B-type stars and red supergiants", Astronomische Nachrichten, 331 (4): 349, arXiv:1003.2335, Bibcode:2010AN....331..349H, doi:10.1002/asna.200911355, S2CID 111387483
  8. [8]
    Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (January 2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun", Monthly Notices of the Royal Astronomical Society, 410 (1): 190–200, arXiv:1007.4883, Bibcode:2011MNRAS.410..190T, doi:10.1111/j.1365-2966.2010.17434.x, S2CID 118629873
  9. [9]
    Tokovinin, Andrei (2018-03-01), "The Updated Multiple Star Catalog", The Astrophysical Journal Supplement Series, 235 (1): 6, arXiv:1712.04750, Bibcode:2018ApJS..235....6T, doi:10.3847/1538-4365/aaa1a5, ISSN 0067-0049, S2CID 119047709
  10. [10]
    "eps Per -- Variable Star of beta Cep type", SIMBAD, Centre de Données astronomiques de Strasbourg, retrieved 2012-01-25
  11. [11]
    "Light Curve", Hipparcos ESA, ESA, retrieved 17 February 2022
  12. [12]
    "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on 2012-03-18, retrieved 2012-01-16
  13. [13]
    Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466–3471, Bibcode:2001AJ....122.3466M, doi:10.1086/323920
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