NN Serpentis

NN Serpentis

Rendering of NN Serpentis system
Observation data
Epoch J2000      Equinox J2000
Constellation Serpens
Right ascension 15h 52m 56.12035s[1]
Declination +12° 54′ 44.4293″[1]
Apparent magnitude (V) +16.51[2]
Characteristics
Spectral type WD DAO1 / M4V[3]
Astrometry
Proper motion (μ) RA: −30.170±0.055 mas/yr[1]
Dec.: −59.084±0.057 mas/yr[1]
Parallax (π)1.9438 ± 0.0662 mas[1]
Distance1,680 ± 60 ly
(510 ± 20 pc)
Orbit[3]
Period (P)0.13008017141(17) d
Semi-major axis (a)0.934 ± 0.009 R☉
Eccentricity (e)0.0
Inclination (i)89.6 ± 0.2°
Semi-amplitude (K1)
(primary)		62.3 ± 1.9 km/s
Semi-amplitude (K2)
(secondary)		301 ± 3 km/s
Details[3]
White dwarf
Mass0.535 ± 0.012 M☉
Radius0.0211 ± 0.0002 R☉
Surface gravity (log g)7.47 ± 0.01 cgs
Temperature57000 ± 3000 K
Red dwarf
Mass0.111 ± 0.004 M☉
Radius0.149 ± 0.002 R☉
Other designations
NN Ser, PG 1550+131, WD 1550+130
Database references
SIMBADdata

NN Serpentis (abbreviated NN Ser) is an eclipsing post-common envelope binary system approximately 1670 light-years away.[3] The system comprises an eclipsing white dwarf and red dwarf. The two stars orbit each other every 0.13 days.[3]

  1. ^ a b c d Cite error: The named reference GaiaDR3 was invoked but never defined (see the help page).
  2. ^ Drake, A. J.; Graham, M. J.; Djorgovski, S. G.; Catelan, M.; Mahabal, A. A.; Torrealba, G.; García-Álvarez, D.; Donalek, C.; Prieto, J. L.; Williams, R.; Larson, S.; Christen Sen, E.; Belokurov, V.; Koposov, S. E.; Beshore, E.; Boattini, A.; Gibbs, A.; Hill, R.; Kowalski, R.; Johnson, J.; Shelly, F. (2014). "The Catalina Surveys Periodic Variable Star Catalog". The Astrophysical Journal Supplement Series. 213 (1): 9. arXiv:1405.4290. Bibcode:2014ApJS..213....9D. doi:10.1088/0067-0049/213/1/9. S2CID 119180446.
  3. ^ a b c d e Cite error: The named reference Parsons was invoked but never defined (see the help page).