Lambda Serpentis,
Latinized from λ Serpentis, is a
star in the
constellationSerpens, in its head (Serpens Caput). It has an
apparent visual magnitude of 4.43,[2] making it visible to the naked eye. Based upon
parallax measurements, this star lies at a distance of about 38.9
light-years (11.9
parsecs) from
Earth.[1] Lambda Serpentis is moving toward the Solar System with a
radial velocity of 66.4 km s−1.[4] In about 166,000 years, this system will make its closest approach of the Sun at a distance of 7.371 ± 0.258 light-years (2.260 ± 0.079 parsecs), before moving away thereafter.[12]
This star is 6% larger and 14% more massive than the Sun, although it has a similar
stellar classification.[1] It is shining with nearly double the Sun's luminosity and this energy is being radiated from the star's outer atmosphere at an
effective temperature of 5,884 K.[9] A periodicity of 1837 days (5.03 years) was suspected by Morbey & Griffith (1987),[13] but it is probably bound to stellar activity. However,
McDonald Observatory team has set limits to the presence of one or more
exoplanets[13] around Lambda Serpentis with masses between 0.16 and 2
Jupiter masses and average separations spanning between 0.05 and 5.2
Astronomical Units.
Planetary system
In 2020, a candidate planet was detected orbiting Lambda Serpentis (HD 141004). With a
minimum mass of 0.043
MJ (13.6
ME) and an orbital period of 15 days, this would most likely be a
hot Neptune.[14] The discovery of planet was confirmed in 2021.[15]
^
abcdJohnson, H. L.; Morgan, W. W. (1953). "Fundamental stellar photometry for standards of spectral type on the revised system of the Yerkes spectral atlas". Astrophysical Journal. 117: 313–352.
Bibcode:
1953ApJ...117..313J.
doi:
10.1086/145697.
S2CID18072563.
^
abFuhrmann, Klaus (October 1998). "Nearby stars of the Galactic disk and halo". Astronomy and Astrophysics. 338: 161–183.
Bibcode:
1998A&A...338..161F.
^Bernacca, P. L.; Perinotto, M. (1970). "A catalogue of stellar rotational velocities". Contributi Osservatorio Astronomico di Padova in Asiago. 239 (1): 1.
Bibcode:
1970CoAsi.239....1B.
^Dybczyński, P. A. (April 2006), "Simulating observable comets. III. Real stellar perturbers of the Oort cloud and their output", Astronomy and Astrophysics, 449 (3): 1233–1242,
Bibcode:
2006A&A...449.1233D,
doi:10.1051/0004-6361:20054284
^
abMorbey, C. L.; Griffith, R. F. (1987). "On the reality of certain spectroscopic orbits". Astrophysical Journal. 317 (1): 343–352.
Bibcode:
1987ApJ...317..343M.
doi:
10.1086/165281.
^
abRosenthal, Lee J.; Fulton, Benjamin J.; Hirsch, Lea A.; Isaacson, Howard T.; Howard, Andrew W.; Dedrick, Cayla M.; Sherstyuk, Ilya A.; Blunt, Sarah C.; Petigura, Erik A.; Knutson, Heather A.; Behmard, Aida; Chontos, Ashley; Crepp, Justin R.; Crossfield, Ian J. M.; Dalba, Paul A.; Fischer, Debra A.; Henry, Gregory W.; Kane, Stephen R.; Kosiarek, Molly; Marcy, Geoffrey W.; Rubenzahl, Ryan A.; Weiss, Lauren M.; Wright, Jason T. (2021), "The California Legacy Survey. I. A Catalog of 178 Planets from Precision Radial Velocity Monitoring of 719 Nearby Stars over Three Decades", The Astrophysical Journal Supplement Series, 255 (1): 8,
arXiv:2105.11583,
Bibcode:
2021ApJS..255....8R,
doi:10.3847/1538-4365/abe23c,
S2CID235186973