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Star in the constellation Lupus
HD 139664
Observation data
Epoch
J2000.0
Equinox
J2000.0 (
ICRS )
Constellation
Lupus
Right ascension
15h 41m 11.3774s
[1]
Declination
−44° 39′ 40.338″
[1]
Apparent magnitude (V)
4.64
[2]
Characteristics
Spectral type
F3/5V
[3]
U−B
color index
−0.03
[4]
B−V
color index
+0.413
[2]
R−I
color index
+0.20
[4]
Astrometry
Radial velocity (Rv ) −7.08± 0.03
[2] km/s
Proper motion (μ)
RA: −168.70
[1]
mas /
yr
Dec.: −265.69
[1]
mas /
yr
Parallax (π) 57.09 ± 0.72
mas
[1]
Distance 57.1 ± 0.7
ly (17.5 ± 0.2
pc )
Absolute magnitude (MV ) 3.57
[5]
Details
[6]
Mass 1.368± 0.026
[2]
M ☉
Radius 1.26
[7]
R ☉
Luminosity 3.31
L ☉
Surface gravity (log g ) 4.29
cgs
Temperature 6,704± 63
K
Rotational velocity (v sin i ) 71.6
[2] km/s
Age 1.11± 1.40
Gyr
Other designations
g Lupi ,
CD −44° 10310 ,
CPD −44° 7529 ,
GC 21070,
GJ 594,
HD 139664,
HIP 76829,
HR 5825,
SAO 226064,
PPM 320883,
LTT 6256,
NLTT 40843
[8]
Database references
SIMBAD
data
HD 139664 is a single
[9]
star in the southern
constellation of
Lupus . It has the
Bayer designation g Lupi ; HD 139664 is the star's identifier from the
Henry Draper Catalogue .
[8] It has a yellow-white hue and is visible to the naked eye with an
apparent visual magnitude of 4.64. The star is located at a distance of 57
light years from the
Sun based on
parallax ,
[1] and it is drifting closer with a
radial velocity of −7 km/s.
[2] It is a member of the Hercules-Lyra Association of co-moving stars.
[10]
[2]
This is an
F-type main-sequence star with a
stellar classification of F3/5V,
[3] which indicates it is generating energy through
core
hydrogen fusion . The estimated age is poorly constrained at around one billion years,
[6] but the age of the Hercules-Lyra Association to which it belongs is 257± 46 million years.
[11] It has a moderately high rate of spin, showing a
projected rotational velocity of 71.6 km/s.
[2] The star has 1.37
[2] times the
mass of the Sun and 1.26
[7] times the
Sun's radius . It is radiating 3.31 times the
luminosity of the Sun from its
photosphere at an
effective temperature of 6,704 K.
[6]
Debris disk
A
debris disk has been imaged around this star using the coronagraphic mode of the
ACS instrument on the
Hubble Space Telescope . The disk appears to have a dust maximum at 83
AU from the star and a sharp outer boundary at 109 AU. These features may be caused by gravitational perturbations from planets orbiting the star.
[12]
References
^
a
b
c
d
e
f van Leeuwen, F. (November 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 .
^
a
b
c
d
e
f
g
h
i Desidera, S.; et al. (January 2015), "The VLT/NaCo large program to probe the occurrence of exoplanets and brown dwarfs in wide orbits. I. Sample definition and characterization", Astronomy & Astrophysics , 573 : 45,
arXiv :
1405.1559 ,
Bibcode :
2015A&A...573A.126D ,
doi :
10.1051/0004-6361/201323168 ,
S2CID
55486025 , A126.
^
a
b Houk, Nancy (1978), Michigan catalogue of two-dimensional spectral types for the HD stars , vol. 2, Ann Arbor: Dept. of Astronomy, University of Michigan,
Bibcode :
1978mcts.book.....H .
^
a
b Hoffleit, D.; Warren, W. H. Jr.,
"HR 5825, database entry" , The Bright Star Catalogue (5th Revised ed.), retrieved February 4, 2011
^ Reiners, Ansgar (January 2006), "Rotation- and temperature-dependence of stellar latitudinal differential rotation", Astronomy and Astrophysics , 446 (1): 267–277,
arXiv :
astro-ph/0509399 ,
Bibcode :
2006A&A...446..267R ,
doi :
10.1051/0004-6361:20053911 ,
S2CID
8642707
^
a
b
c Luck, R. Earle (March 2018), "Abundances in the Local Region. III. Southern F, G, and K Dwarfs", The Astronomical Journal , 155 (3): 31,
Bibcode :
2018AJ....155..111L ,
doi :
10.3847/1538-3881/aaa9b5 ,
S2CID
125765376 , 111.
^
a
b Rhee, Joseph H.; et al. (May 2007), "Characterization of Dusty Debris Disks: The IRAS and Hipparcos Catalogs", The Astrophysical Journal , 660 (2): 1556–1571,
arXiv :
astro-ph/0609555 ,
Bibcode :
2007ApJ...660.1556R ,
doi :
10.1086/509912 ,
S2CID
11879505 .
^
a
b
"g Lup" .
SIMBAD .
Centre de données astronomiques de Strasbourg . Retrieved 2020-07-01 .
^ Halbwachs, J. -L; et al. (2018), "Multiplicity among solar-type stars. IV. The CORAVEL radial velocities and the spectroscopic orbits of nearby K dwarfs", Astronomy and Astrophysics , 619 : A81,
arXiv :
1808.04605 ,
Bibcode :
2018A&A...619A..81H ,
doi :
10.1051/0004-6361/201833377 ,
S2CID
119437322 .
^ Lopez-Santiago, J.; et al. (2006), "The Nearest Young Moving Groups",
The Astrophysical Journal , 643 (2): 1160–1165,
arXiv :
astro-ph/0601573 ,
Bibcode :
2006ApJ...643.1160L ,
doi :
10.1086/503183 ,
S2CID
119520529 .
^ Eisenbeiss, T.; et al. (August 2013), "The Hercules-Lyra association revisited. New age estimation and multiplicity study", Astronomy & Astrophysics , 556 : 19,
arXiv :
1312.4045 ,
Bibcode :
2013A&A...556A..53E ,
doi :
10.1051/0004-6361/201118362 ,
S2CID
119275785 , A53.
^ Kalas, Paul; et al. (January 2006),
"First Scattered Light Images of Debris Disks around HD 53143 and HD 139664" , The Astrophysical Journal , 637 (1): L57–L60,
arXiv :
astro-ph/0601488 ,
Bibcode :
2006ApJ...637L..57K ,
doi :
10.1086/500305 ,
S2CID
18293244 .