Zeta Serpentis

Zeta Serpentis

Observation data Epoch J2000      Equinox J2000
Constellation	Serpens
Right ascension	18^h 00^m 29.0^s[1] [2]
Declination	−03° 41′ 25″[1] [2]
Apparent magnitude (V)	4.63 [3]
Characteristics
Spectral type	F2V [4]
B−V color index	+0.36 [3]
Astrometry
Radial velocity (Rv)	-50.70[5] km/s
Proper motion (μ)	RA: +155.51[2] mas/yr Dec.: -44.43[2] mas/yr
Parallax (π)	42.46 ± 0.34[2] mas
Distance	76.8 ± 0.6 ly (23.6 ± 0.2 pc)
Absolute magnitude (MV)	2.77 [6]
Other designations
57 Serpentis, GC 24503, HIP 88175, HR 6710, HD 164259, SAO 142025 [3]
Database references
SIMBAD	data

Zeta Serpentis (ζ Ser, ζ Serpentis) is a star in the constellation Serpens.

Zeta Serpentis is a yellow-white F-type main sequence dwarf with an apparent magnitude of +4.63.^[3] It is approximately 76.8 light years from Earth.^[2] This star has nearly double the radius of the Sun and is radiating 6.3 times the Sun's luminosity from its outer atmosphere at an effective temperature of 6,529 K.^[1]

References

1. Boyajian, Tabetha S.; et al. (February 2012), "Stellar Diameters and Temperatures. I. Main-sequence A, F, and G Stars", The Astrophysical Journal 746 (1): 101, arXiv:1112.3316, Bibcode:2012ApJ...746..101B, doi:10.1088/0004-637X/746/1/101. See Table 10.
2. 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. Vizier catalog entry
3. "Zeta Serpentis". SIMBAD Astronomical Database. Retrieved 2015-10-17.
4. Gray, R. O.; et al. (October 2003), "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 Parsecs: The Northern Sample. I.", The Astronomical Journal 126 (4): 2048–2059, arXiv:astro-ph/0308182, Bibcode:2003AJ....126.2048G, doi:10.1086/378365
5. Gontcharov, G. A. (November 2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters 32 (11): 759–771. Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065.
6. Absolute magnitude calculated as $M = m + 5 (1 + \log_{10}{p})\!\,$, where $M$ is the star's absolute magnitude, $m$ is the star's apparent magnitude, and $p$ is the star's measured parallax in arcseconds.