Star in the constellation Lyra
WASP-3
Observation dataEpoch J2000.0 Equinox J2000.0
Constellation
Lyra [ 2]
WASP-3A
Right ascension
18h 34m 31.6252s [ 3]
Declination
+35° 39′ 41.492″[ 3]
Apparent magnitude (V)
10.63± 0.05[ 4]
WASP-3C
Right ascension
18h 34m 30.2553s [ 5] [ 6]
Declination
+35° 39′ 34.004″[ 5] [ 6]
Characteristics
WASP-3A
Evolutionary stage
main-sequence star
Spectral type
F7V[ 4]
Apparent magnitude (B)
11.07± 0.06[ 4]
Apparent magnitude (G)
10.4541± 0.0028[ 4] [ 6]
Apparent magnitude (J)
9.603± 0.020[ 4]
Apparent magnitude (H)
9.407± 0.014[ 4]
Apparent magnitude (K)
9.361± 0.015[ 4]
Variable type
planetary transit [ 7]
WASP-3B
Apparent magnitude (J)
16.88± 0.12[ 8]
Apparent magnitude (H)
16.090± 0.079[ 8]
Apparent magnitude (K)
16.002± 0.052[ 8]
Astrometry WASP-3A Radial velocity (Rv ) −5.490± 0.007[ 9] km/s Proper motion (μ) RA: −5.791(12) mas /yr [ 3] Dec.: −21.929(15) mas /yr [ 3] Parallax (π)4.3338± 0.0120 mas [ 3] Distance 753 ± 2 ly (230.7 ± 0.6 pc )
Details WASP-3A Mass 1.24+0.06 −0.11 [ 9] : 1581 M ☉ Radius 1.366± 0.044[ 10] R ☉ Surface gravity (log g ) 4.30+0.07 −0.03 [ 9] : 1581 cgs Temperature 6400± 100[ 9] : 1581 K Metallicity 0.00± 0.20[ 9] : 1581 Rotational velocity (v sin i ) 13.4± 1.5[ 10] km/sAge 2.1± 1.2[ 10] Gyr WASP-3B Mass 0.108± 0.006[ 8] : 14 M ☉ Surface gravity (log g )~5.22[ 8] : 13 cgs Temperature ~2900[ 8] : 13 K
Position (relative to WASP-3A) [ 8] : 11, 14
Component WASP-3B Epoch of observation 2012–2013 Angular distance ~1.19″ Position angle ~87.1° Projected separation 300± 20 AU
Position (relative to WASP-3A) [ 6]
Component WASP-3C Angular distance 18.33192 ± 0.00002 ″ Position angle 245.81872 ± 0.00006 ° Projected separation 4230 AU
Other designations V838 Lyr , BD +35 3293 , TOI -2131 , TIC 27848472 , WASP -3 , TYC 2636-195-1 , GSC 02636-00195 , 2MASS J18343163+3539415 , USNO-B1.0 1256-00285133, 1SWASP J183431.62+353941.4[ 4]
Database references SIMBAD data Exoplanet Archive data
WASP-3 is a triple star system located about 753 light-years (231 parsecs ) away from the Sun in the constellation Lyra . The system has an apparent magnitude of 10. The brightest and most massive star of this system is WASP-3A, an F-type main sequence star which has one known transiting hot Jupiter exoplanet , WASP-3b . Since the planet transits the star, the star is classified as a planetary transit variable and has received the variable star designation V838 Lyrae .[ 7]
Triple system
WASP-3 has been identified as a triple star system in a 2019 study of astrometry from the Gaia mission.[ 11] : 5093 The brightest and most massive component of the system is WASP-3A, an F-type main sequence star that is 1.24 times as massive as the Sun and 1.31 times as large as the Sun in radius.[ 9] : 1581 WASP-3A appears to be a variable star ; observations between 2007 and 2010 show that the star's chromospheric activity had increased during that time period.[ 12] The second companion, WASP-3B, is a low-mass star about 0.11 times as massive as the Sun and has an effective temperature of about 2900 K .[ 8] : 11, 13 WASP-3B is separated eastward from WASP-3A at an angular separation of approximately 1.19 arcseconds , corresponding to a projected separation distance of about 300 AU .[ 8] : 11, 13 WASP-3B was first identified in observations from 2012 to 2013.[ 8] : 14 The third companion, WASP-3C, is much more distant with an angular separation of approximately 18.3 arcseconds from WASP-3A, corresponding to a projected separation distance of 4230 AU .[ 11] : 5093 WASP-3C is about 0.77 times as massive as the Sun and has an effective temperature of about 4700 K .[ 6]
Planetary system
WASP-3A has one known transiting hot Jupiter extrasolar planet , WASP-3b , which was detected by the SuperWASP project in 2007.[ 9] It was confirmed in 2008 by observations from the William Herschel Telescope .
In 2010, researchers proposed a second planet orbiting WASP-3A due to transit timing variations in WASP-3b.[ 13] [ 14] But in 2012 this proposal was refuted.[ 12]
See also
References
^ "MAST: Barbara A. Mikulski Archive for Space Telescopes" . Space Telescope Science Institute. Retrieved 11 April 2025 .
^ Roman, Nancy G. (1987). "Identification of a constellation from a position" . Publications of the Astronomical Society of the Pacific . 99 (617): 695. Bibcode :1987PASP...99..695R . doi :10.1086/132034 .
Constellation record for this object at VizieR .
^ a b c d Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties" . Astronomy and Astrophysics . 674 : A1. arXiv :2208.00211 . Bibcode :2023A&A...674A...1G . doi :10.1051/0004-6361/202243940 . S2CID 244398875 .
Gaia DR3 record for this source at VizieR .
^ a b c d e f g h "TYC 2636-195-1" . SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2009-05-04 .
^ a b "UCAC4 629-058739" . SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 23 March 2025 .
^ a b c d e Michel, Kai-Uwe; Mugrauer, Markus (January 2024). "Gaia search for (sub)stellar companions of exoplanet hosts (Supplementary file)" . Monthly Notices of the Royal Astronomical Society . 527 (2): 3183– 3195. Bibcode :2024MNRAS.527.3183M . doi :10.1093/mnras/stad3196 .
^ a b "V838 Lyr" . General Catalog of Variable Stars - VizieR . Retrieved 3 April 2025 .
^ a b c d e f g h i j Ngo, Henry; Knutson, Heather A.; Hinkley, Sasha; Crepp, Justin R.; Bechter, Eric B.; Batygin, Konstantin; et al. (February 2015). "Friends of Hot Jupiters. II. No Correspondence between Hot-jupiter Spin-Orbit Misalignment and the Incidence of Directly Imaged Stellar Companions" . The Astrophysical Journal . 800 (2): 22. arXiv :1501.00013 . Bibcode :2015ApJ...800..138N . doi :10.1088/0004-637X/800/2/138 . 138.
^ a b c d e f g Pollacco, D.; et al. (2008). "WASP-3b: a strongly irradiated transiting gas-giant planet" . Monthly Notices of the Royal Astronomical Society . 385 (3): 1576– 1584. arXiv :0711.0126 . Bibcode :2008MNRAS.385.1576P . doi :10.1111/j.1365-2966.2008.12939.x . S2CID 2317308 .
^ a b c d Bonomo, A. S.; Desidera, S.; et al. (June 2017). "The GAPS Programme with HARPS-N at TNG. XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets". Astronomy & Astrophysics . 602 : A107. arXiv :1704.00373 . Bibcode :2017A&A...602A.107B . doi :10.1051/0004-6361/201629882 .
^ a b Mugrauer, M. (December 2019). "Search for stellar companions of exoplanet host stars by exploring the second ESA-Gaia data release" . Monthly Notices of the Royal Astronomical Society . 490 (4): 5088– 5102. Bibcode :2019MNRAS.490.5088M . doi :10.1093/mnras/stz2673 .
^ a b M Montalto; Gregorio, J.; Boue, G.; Mortier, A.; Boisse, I.; Oshagh, M.; Maturi, M.; Figueira, P.; Sousa, S.; Santos, N. C. (Nov 2, 2012). "A new analysis of the WASP-3 system: no evidence for an additional companion" . MNRAS . 427 (4): 2757. arXiv :1211.0218 . Bibcode :2012MNRAS.427.2757M . doi :10.1111/j.1365-2966.2012.21926.x . S2CID 59381004 .
^ Planet found tugging on transits Archived 2010-07-13 at the Wayback Machine , Astronomy Now, 9 July 2010
^ G.Maciejewski; D.Dimitrov; R.Neuhaeuser; A.Niedzielski; St.Raetz; Ch.Ginski; Ch.Adam, C.Marka; M.Moualla; M.Mugrauer (2010). "Transit timing variation in exoplanet WASP-3b" . Monthly Notices of the Royal Astronomical Society . 407 (4): 2625– 2631. arXiv :1006.1348 . Bibcode :2010MNRAS.407.2625M . doi :10.1111/j.1365-2966.2010.17099.x . S2CID 120998224 .
External links