Psi Serpentis
| Observation data ICRS )
| ||
|---|---|---|
| Constellation | Serpens | |
| Right ascension | 15h 44m 01.82075s[1] | |
| Declination | +02° 30′ 54.6340″[1] | |
| Apparent magnitude (V) | 5.84[2] + 12.00[3] | |
| Characteristics | ||
| Spectral type | G5 V[4] + (M3 + M3)[5] | |
| U−B color index | +0.23[2] | |
| B−V color index | +0.68[2] | |
| Absolute magnitude (MV) | +5.03[4] | |
Argument of periastron (ω)(secondary) | 330.9 ± 3.4° | |
Argument of periastron (ω)(secondary) | 230.0 ± 9.3° | |
| Details Gyr | ||
| ψ Ser Ba | ||
| Mass | 0.26[7] M☉ | |
| ψ Ser Bb | ||
| Mass | 0.24[7] M☉ | |
| Database references | ||
| SIMBAD | data | |
Psi Serpentis (ψ Ser, ψ Serpentis) is a
apparent visual magnitude of 5.84.[2]
This system can be resolved into two components that orbit each other with a
solar twin.[4] The star has an estimated 99.3% of the mass of the Sun,[6] and it matches the Sun's radius within the margin of error.[8] It is radiating 98%[9] of the solar luminosity from its photosphere at an effective temperature of 5,683 K.[6]
When observed from 1997 through 2000, the primary component appeared to be transitioning from a
star spot-dominated variations in luminosity.[15]
The known secondary, component B, is magnitude 12.00 and lies at an
AU. Both components, Ba and Bb, are likely red dwarfs roughly of class M3[5] with masses close to a quarter of that of the Sun.[7] Their orbital period is estimated to be 6.57 years, and the eccentricity is moderately high, at 0.357.[7] The orbit of Ba and Bb is not coplanar to their orbit around A.[7]
References
- ^ S2CID 18759600.
- ^ Bibcode:1986EgUBV........0M.
- ^ doi:10.1086/323920.
- ^ S2CID 119205608, A131.
- ^ S2CID 119237891.
- ^ S2CID 46964342, A48.
- ^ S2CID 231419112
- ^ S2CID 18775378.
- ^ S2CID 118665352.
- S2CID 43455849, archived from the original(PDF) on 2017-09-22, retrieved 2018-11-04.
- ^ "psi Ser". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-03-23.
{{cite web}}: CS1 maint: postscript (link) - S2CID 59039482, A35.
- ^ Gatewood, G.; Mason, B. D. (2013), Information Circular No. 181 (PDF), International Astronomical Union Commission 26 (Double Stars), p. 1, archived from the original (PDF) on 2016-12-21, retrieved 2017-03-25.
- doi:10.1086/510356.
- S2CID 12332945.