Electra
Image of the Pleiades star cluster
Electra in the Pleiades cluster (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Taurus
Right ascension 03h 44m 52.53688s[1]
Declination +24° 06′ 48.0112″[1]
Apparent magnitude (V) 3.70[2]
Characteristics
Spectral type B6 IIIe[3]
U−B color index -0.40[4]
B−V color index -0.12[4]
Astrometry
Radial velocity (Rv)+10.9[5] km/s
Proper motion (μ) RA: +20.84[1] mas/yr
Dec.: −46.06[1] mas/yr
Parallax (π)8.06 ± 0.25 mas[1]
Distance400 ± 10 ly
(124 ± 4 pc)
Absolute magnitude (MV)−1.77[6]
Details
Mass4.6-4.7[7] M☉
Radius6.06+0.14
−0.15[8] R☉
Luminosity940[8] L☉
Surface gravity (log g)3.412±0.047[9] cgs
Temperature13,484±293[9] K
Rotational velocity (v sin i)181[9] km/s
Age115[10] Myr
Other designations
17 Tauri, BD+23 507, FK5 136, GC 4477, HD 23302, HIP 17499, HR 1142, SAO 76131, NSV 15755
Database references
SIMBADdata

Electra /əˈlɛktrə/,[11] designated 17 Tauri, is a blue-white giant star in the constellation of Taurus, about 400 light years away. It is the third-brightest star in the Pleiades open star cluster (M45), visible to the naked eye with an apparent magnitude of 3.7. Like the other bright stars of the Pleiades, it is named for one of the Seven Sisters of Greek mythology.

Properties

The Pleiades Cluster in infrared with Electra at the very top of the frame

Electra has an apparent brightness of 3.72, the third-brightest of the stars in the group. It belongs to the spectral class B6 IIIe and is approximately 400 light-years from the Sun.[1] The Pleiades cluster is thought to be 444 light-years away. A number of papers have reported Electra to be a multiple star, but these have been contradictory and never confirmed.[12]

The projected rotational velocity of this star is 181 km/s, making it a fast rotator. This is the velocity component of the star's equatorial rotation along the line of sight to the Earth. The estimated inclination of the star's pole is 46.8°±1.6°, giving it a true equatorial rotational velocity of 320±18 km/s. The rapid rotation rate of this star flattens the poles and stretch the equator. This makes the surface gravity of the star non-uniform and causes temperature variation. This effect is known as gravity darkening, because it results in a variation of radiation by latitude. The rapid rotation extends the life span of the star by increasing the core density and reducing the radiation output.[9]

This is classified as a Be star, which is a B-type star with prominent emission lines of hydrogen in its spectrum.[3] The Be stars have a rotation rate that is 1.5–2 times the rotation of normal B-type stars. This high rate of rotation may allow mass loss during even minor prominences.[7] Changes in the radial velocity measurements indicate that this star may have a companion, which would make Electra a spectroscopic binary.[13][14] However, follow-up studies including interferometry have failed to confirm any companion star(s), so it is likely a single star.[15]

A light curve for Electra, adapted from White et al. (2017)[16]

Electra may be a variable star, and it appears in the New Catalogue of Suspected Variable Stars as NSV 15755. Low amplitude variability of the brightness of Electra was detected by Kepler/K2, and Fourier analysis of the star's light curve shows several periods of oscillation, the strongest being 1.107 and 1.165 days.[16] The International Variable Star Index classifies it as a slowly pulsating B star.[17]

Infrared observations of this star showed an excess level of radiation equal to about 0.5 magnitudes. This emission is probably from a gaseous disk created by radiation-driven mass loss and rapid rotation of the star. These disks are created by an ejection of material roughly every ten years, which then settles into the equatorial plane about the star. However, the bright nebulosity that surrounds this star makes the observation uncertain.[18]

Nomenclature

17 Tauri is the star's Flamsteed designation.

It bore the traditional name Electra.[19] Electra was one of the Pleiades sisters in Greek mythology. In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[20] to catalogue and standardize proper names for stars. The WGSN approved the name Electra for this star on 21 August 2016 and it is now so entered in the IAU Catalog of Star Names.[21]

Military namesakes

USS Electra (1843) and USS Electra (AK-21/AKA-4), were both ships of the United States Navy.

References

  1. 1 2 3 4 5 6 Van Leeuwen, F. (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. ↑ Ducati, J. R (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D.
  3. 1 2 Grady, C. A.; Bjorkman, K. S.; Snow, T. P.; Sonneborn, George; Shore, Steven N.; Barker, Paul K. (April 1989). "Highly ionized stellar winds in Be stars. II - Winds in B6-B9.5e stars". Astrophysical Journal, Part 1. 339: 403–419. Bibcode:1989ApJ...339..403G. doi:10.1086/167306.
  4. 1 2 Johnson, H. L.; Iriarte, B.; Mitchell, R. I.; Wisniewskj, W. Z. (1966). "UBVRIJKL photometry of the bright stars". Communications of the Lunar and Planetary Laboratory. 4: 99–110. Bibcode:1966CoLPL...4...99J.
  5. ↑ Pearce, J. A.; Hill, G. (1975). "A spectroscopic investigation of the Pleiades". Publications of the Dominion Astrophysical Observatory. 14 (14): 319–343. Bibcode:1975PDAO...14..319P.
  6. ↑ Zhang, P; Liu, C. Q; Chen, P. S (2006). "Absolute Magnitudes of Be Stars Based on Hipparcos Parallaxes". Astrophysics and Space Science. 306 (3): 113. Bibcode:2006Ap&SS.306..113Z. doi:10.1007/s10509-006-9173-1. S2CID 122897957.
  7. 1 2 Zorec, J.; Frémat, Y.; Cidale, L. (October 2005). "On the evolutionary status of Be stars. I. Field Be stars near the Sun". Astronomy and Astrophysics. 441 (1): 235–248. arXiv:astro-ph/0509119. Bibcode:2005A&A...441..235Z. doi:10.1051/0004-6361:20053051. S2CID 17592657.
  8. 1 2 Harmanec, P (2000). "Physical Properties and Evolutionary Stage of Be Stars". The be Phenomenon in Early-Type Stars. 214: 13. Bibcode:2000ASPC..214...13H.
  9. 1 2 3 4 Frémat, Y.; Zorec, J.; Hubert, A.-M.; Floquet, M. (September 2005). "Effects of gravitational darkening on the determination of fundamental parameters in fast-rotating B-type stars". Astronomy and Astrophysics. 440 (1): 305–320. arXiv:astro-ph/0503381. Bibcode:2005A&A...440..305F. doi:10.1051/0004-6361:20042229. S2CID 19016751.
  10. ↑ Basri, Gibor; Marcy, Geoffrey W.; Graham, James R. (1996). "Lithium in Brown Dwarf Candidates: The Mass and Age of the Faintest Pleiades Stars". The Astrophysical Journal. 458: 600–609. Bibcode:1996ApJ...458..600B. doi:10.1086/176842.
  11. ↑ "Electra". Oxford English Dictionary (Online ed.). Oxford University Press. (Subscription or participating institution membership required.)
  12. ↑ Hutter, D. J.; Tycner, C.; Zavala, R. T.; Benson, J. A.; Hummel, C. A.; Zirm, H. (2021). "Surveying the Bright Stars by Optical Interferometry. III. A Magnitude-limited Multiplicity Survey of Classical be Stars". The Astrophysical Journal Supplement Series. 257 (2): 69. arXiv:2109.06839. Bibcode:2021ApJS..257...69H. doi:10.3847/1538-4365/ac23cb. S2CID 237503492.
  13. ↑ Abt, Helmut A.; Barnes, Ronnie C.; Biggs, Eleanor S.; Osmer, Patrick S. (November 1965). "The Frequency of Spectroscopic Binaries in the Pleiades". Astrophysical Journal. 142: 1604–1615. Bibcode:1965ApJ...142.1604A. doi:10.1086/148440. S2CID 121363965.
  14. ↑ Pearce, J. A.; Hill, Graham (1971). "Four Suspected Spectroscopic Binaries in the Pleiades". Publications of the Astronomical Society of the Pacific. 83 (494): 493–495. Bibcode:1971PASP...83..493P. doi:10.1086/129161.
  15. ↑ Hutter, D. J.; Tycner, C.; Zavala, R. T.; Benson, J. A.; Hummel, C. A.; Zirm, H. (2021). "Surveying the Bright Stars by Optical Interferometry. III. A Magnitude-limited Multiplicity Survey of Classical Be Stars". The Astrophysical Journal Supplement Series. 257 (2): 69. arXiv:2109.06839. Bibcode:2021ApJS..257...69H. doi:10.3847/1538-4365/ac23cb. S2CID 237503492.
  16. 1 2 White, T. R.; et al. (November 2017). "Beyond the Kepler/K2 bright limit: variability in the seven brightest members of the Pleiades". Monthly Notices of the Royal Astronomical Society. 471 (3): 2882–2901. arXiv:1708.07462. Bibcode:2017MNRAS.471.2882W. doi:10.1093/mnras/stx1050.
  17. ↑ "NSV 15755". The International Variable Star Index. AAVSO. Retrieved 8 October 2022.
  18. ↑ Gorlova, Nadya; Rieke, George H.; Muzerolle, James; Stauffer, John R.; Siegler, Nick; Young, Erick T.; Stansberry, John H. (October 2006). "Spitzer 24 μm Survey of Debris Disks in the Pleiades". The Astrophysical Journal. 649 (2): 1028–1042. arXiv:astro-ph/0606039. Bibcode:2006ApJ...649.1028G. doi:10.1086/506373. S2CID 17227369.
  19. ↑ Allen, Richard Hinckley (1899). Star-names and their meanings. G. E. Stechert. p. 406. Retrieved 2009-10-10.
  20. ↑ "IAU Working Group on Star Names (WGSN)". International Astronomical Union. Retrieved 22 May 2016.
  21. ↑ "IAU Catalog of Star Names". Retrieved 28 July 2016.
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