BD-07 436

Last updated
BD-07 436
Observation data
Epoch J2000       Equinox J2000
Constellation Cetus
Right ascension 02h 28m 37.226s [1]
Declination −07° 03 38.39 [1]
Apparent magnitude  (V)10.12
Characteristics
Evolutionary stage main-sequence star
Spectral type G8+K5 [2]
Astrometry
Proper motion (μ)RA: 88 [1]   mas/yr
Dec.: 8.1 [1]   mas/yr
Parallax (π)9.4818 ± 0.1073  mas [3]
Distance 344 ± 4  ly
(105 ± 1  pc)
Orbit [2] [4]
PrimaryBD-07 436A
CompanionBD-07 436B
Semi-major axis (a)3.3"
(461+200
140
AU)
Eccentricity (e)0.51+0.26
0.22
Inclination (i)77+5
7
°
Details [5]
BD-07 436A
Mass 0.903+0.066
0.059
  M
Radius 0.910+0.025
0.023
  R
Luminosity 0.743+0.065
0.058
  L
Surface gravity (log g)4.476+0.014
0.015
  cgs
Temperature 5617±72  K
Metallicity [Fe/H]−0.10+0.10
0.11
  dex
Rotation 15.4±0.5 [6]
Rotational velocity (v sin i)4.0±0.2 km/s
Age 5 [2]   Gyr
BD-07 436B
Mass 0.71±0.06 [7]   M
Radius 0.69±0.12 [7]   R
Surface gravity (log g)4.6±0.15 [7]   cgs
Temperature 5570±240 [4]   K
Metallicity [Fe/H]-0.11±0.19 [7]   dex
Rotational velocity (v sin i)2.8±0.5 [7]  km/s
Age >9 [2]   Gyr
Other designations
Gaia DR2  5178405479960844160, TOI-398, WASP-77, TYC  4697-201-1, 2MASS J02283722-0703384 [1]
Database references
SIMBAD 436 data

BD-07 436, also known as WASP-77 since 2012, [7] is a binary star system about 344 light-years away. The star's components appears to have a different age, with the secondary older than 9 billion years, while the primary's age is 5 billion years. [2] The BD-07 436 system's concentration of heavy elements is similar to the Sun. Its stars display moderate chromospheric activity, including x-ray flares. [2]

The primary is a G-type main-sequence star, BD-07 436A (WASP-77A). The star is rotating rapidly, being spun up by the tides raised by the giant planet WASP-77Ab on its close orbit. [6] The secondary is a K-type main-sequence star BD-07 436B orbiting at a distance of 461+200
140
AU. [4]

Planetary system

In 2012 a transiting hot Jupiter planet b was detected on a very tight, circular orbit. [7] The planet may have an extended gaseous envelope and is losing mass. [2] Its equilibrium temperature is 1715+26
25
K, [5] the nightside temperature measured in 2019 is 1786±84 K, [8] and dayside planetary temperature measured in 2020 is 1842+34
33
K. [9]

Water vapour was detected on the planetary dayside of WASP-77Ab, indicating C/O ratio similar to solar or even lower. [10]

The BD-07 436A planetary system [5]
Companion
(in order from star)
Mass Semimajor axis
(AU)
Orbital period
(days)
Eccentricity Inclination Radius
Ab 1.667+0.068
0.064
  MJ
0.02335+0.00045
0.00043
1.36002854±0.000000620.0074+0.0069
0.0049
88.91+0.74
0.95
°
1.230+0.031
0.029
  RJ

Related Research Articles

<span class="mw-page-title-main">WASP-4b</span> Extrasolar planet in the constellation Phoenix

WASP-4b is an extrasolar planet approximately 891 light-years away in the constellation of Phoenix.

<span class="mw-page-title-main">WASP-4</span> G-type main sequence star in the constellation Phoenix

WASP-4 is a G-type main sequence star approximately 891 light-years away in the constellation of Phoenix. Despite its advanced age, the star is rotating rapidly, being spun up by the tides raised by a giant planet on close orbit.

<span class="mw-page-title-main">WASP-43b</span> Extrasolar planet in the constellation Sextans

WASP-43b, formally named Astrolábos, is a transiting planet in orbit around the young, active, and low-mass star WASP-43 in the constellation Sextans. The planet is a hot Jupiter with a mass twice that of Jupiter, but with a roughly equal radius. WASP-43b was flagged as a candidate by the SuperWASP program, before they conducted follow-ups using instruments at La Silla Observatory in Chile, which confirmed its existence and provided orbital and physical characteristics. The planet's discovery was published on April 14, 2011.

WASP-36 is a yellow main sequence star in the Hydra constellation.

Qatar-1 is an orange main sequence star in the constellation of Draco.

WASP-46 is a G-type main-sequence star about 1,210 light-years away. The star is older than the Sun and is strongly depleted in heavy elements compared to the Sun, having just 45% of the solar abundance. Despite its advanced age, the star is rotating rapidly, being spun up by the tides raised by a giant planet on a close orbit.

WASP-35 is a G-type main-sequence star about 660 light-years away. The star's age cannot be well constrained, but it is probably older than the Sun. WASP-35 is similar in concentration of heavy elements compared to the Sun.

WASP-78, is a single F-type main-sequence star about 2500 light-years away. It is likely to be younger than the Sun at 3.4+1.5
−0.8
billion years. WASP-78 is depleted in heavy elements, having a 45% concentration of iron compared to the Sun.

WASP-72 is the primary of a binary star system. It is an F7 class dwarf star, with an internal structure just on the verge of the Kraft break. It is orbited by a planet WASP-72b. The age of WASP-72 is younger than the Sun at 3.55±0.82 billion years.

WASP-64 is a star about 1200 light-years away. It is a G7 class main-sequence star, orbited by a planet WASP-64b. It is younger than the Sun at 3.6±1.6 billion years, and it has a metal abundance similar to the Sun. The star is rotating rapidly, being spun up by the giant planet in a close orbit.

WASP-67 is a K-type main-sequence star about 620 light-years away. The stars age is poorly constrained, but is likely older than the Sun`s at approximately 8.7+5.5
−8.6
billion years. WASP-67 is slightly depleted in heavy elements, having 85% of the solar abundance of iron.

WASP-63 or Kosjenka, also known as CD-38 2551, is a single star with an exoplanetary companion in the southern constellation of Columba. It is too faint to be visible with the naked eye, having an apparent visual magnitude of 11.1. The distance to this system is approximately 942 light-years based on parallax measurements, but it is drifting closer with a radial velocity of −24 km/s.

WASP-55 is a G-type main-sequence star about 980 light-years away. The star is much younger than the Sun at approximately 1.1+0.8
−0.6
 billion years
. WASP-55 is similar to the Sun in concentration of heavy elements.

WASP-52 is a K-type main-sequence star about 570 light-years away. It is older than the Sun at 10.7+1.9
−4.5
billion years, but it has a similar fraction of heavy elements. The star has prominent starspot activity, with 3% to 14% of the stellar surface covered by areas 575±150 K cooler than the rest of the photosphere.

WASP-41 is a G-type main-sequence star. Its surface temperature is 5450±150 K. WASP-41 is similar to the Sun in its concentration of heavy elements, with a metallicity Fe/H index of −0.080±0.090, but is much younger at an age of 2.289±0.077 billion years. The star does exhibit strong starspot activity, with spots covering 3% of the stellar surface.

HAT-P-41 is a binary star system. Its primary is a F-type main-sequence star. Its surface temperature is 6390±100 K. compared to the Sun, HAT-P-41 is enriched in heavy elements, with a metallicity Fe/H index of 0.21±0.10, but is much younger at an age of 2.2±0.4 billion years.

WASP-84, also known as BD+02 2056, is a G-type main-sequence star 327 light-years away in the constellation Hydra. Its surface temperature is 5350±31 K and is slightly enriched in heavy elements compared to the Sun, with a metallicity Fe/H index of 0.05±0.02. It is rich in carbon and depleted of oxygen. WASP-84's age is probably older than the Sun at 8.5+4.1
−5.5
billion years. The star appears to have an anomalously small radius, which can be explained by the unusually high helium fraction or by it being very young.

WASP-80 is a K-type main-sequence star about 162 light-years away. The star's age is much younger than the Sun's at 1.352±0.222 billion years. WASP-80 is similar to the Sun in concentration of heavy elements, although this measurement is highly uncertain.

WASP-103 is an F-type main-sequence star located 1,800 ± 100 light-years away in the constellation Hercules. Its surface temperature is 6,110±160 kelvins (K). The star's concentration of heavy elements is similar to that of the Sun. WASP-103 is slightly younger than the Sun at 4±1 billion years. The chromospheric activity of the star is elevated due to interaction with the giant planet on a close-in orbit.

References

  1. 1 2 3 4 5 "BD-07 436". SIMBAD . Centre de données astronomiques de Strasbourg.
  2. 1 2 3 4 5 6 7 Salz, M.; Schneider, P. C.; Czesla, S.; Schmitt, J. H. M. M. (2015), "High-energy irradiation and mass loss rates of hot Jupiters in the solar neighborhood", Astronomy & Astrophysics, 576: A42, arXiv: 1502.00576 , Bibcode:2015A&A...576A..42S, doi:10.1051/0004-6361/201425243, S2CID   55139248
  3. Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
  4. 1 2 3 Evans, D. F.; Southworth, J.; Smalley, B.; Jørgensen, U. G.; Dominik, M.; Andersen, M. I.; Bozza, V.; Bramich, D. M.; Burgdorf, M. J.; Ciceri, S.; d'Ago, G.; Figuera Jaimes, R.; Gu, S.-H.; Hinse, T. C.; Henning, Th.; Hundertmark, M.; Kains, N.; Kerins, E.; Korhonen, H.; Kokotanekova, R.; Kuffmeier, M.; Longa-Peña, P.; Mancini, L.; MacKenzie, J.; Popovas, A.; Rabus, M.; Rahvar, S.; Sajadian, S.; Snodgrass, C.; et al. (2018), "High-resolution Imaging of Transiting Extrasolar Planetary systems (HITEP). II. Lucky Imaging results from 2015 and 2016", Astronomy & Astrophysics, 610: A20, arXiv: 1709.07476 , Bibcode:2018A&A...610A..20E, doi:10.1051/0004-6361/201731855, S2CID   53400492
  5. 1 2 3 Cortes-Zuleta, Pia; Rojo, Patricio; Wang, Songhu; Hinse, Tobias C.; Hoyer, Sergio; Sanhueza, Bastian; Correa-Amaro, Patricio; Albornoz, Julio (2020), "TraMoS V. Updated ephemeris and multi-epoch monitoring of the hot Jupiters WASP-18Ab, WASP-19b, and WASP-77Ab", Astronomy & Astrophysics, A98: 636, arXiv: 2001.11112 , Bibcode:2020A&A...636A..98C, doi:10.1051/0004-6361/201936279, S2CID   210966021
  6. 1 2 Gallet, F.; Gallet (2020), "TATOO: Tidal-chronology standalone tool to estimate the age of massive close-in planetary systems", Astronomy & Astrophysics, 641: A38, arXiv: 2006.07880 , Bibcode:2020A&A...641A..38G, doi:10.1051/0004-6361/202038058, S2CID   219687851
  7. 1 2 3 4 5 6 7 Maxted, P. F. L.; Anderson, D. R.; Collier Cameron, A.; Doyle, A. P.; Fumel, A.; Gillon, M.; Hellier, C.; Jehin, E.; Lendl, M.; Pepe, F.; Pollacco, D. L.; Queloz, D.; Ségransan, D.; Smalley, B.; Southworth, K.; Smith, A. M. S.; Triaud, A. H. M. J.; Udry, S.; West, R. G. (2012), "WASP-77 Ab: A transiting hot Jupiter planet in a wide binary system", Publications of the Astronomical Society of the Pacific, 125 (923): 48–55, arXiv: 1211.6033 , doi:10.1086/669231, S2CID   53552999
  8. Garhart, Emily; Deming, Drake; Mandell, Avi; Knutson, Heather A.; Wallack, Nicole; Burrows, Adam; Fortney, Jonathan J.; Hood, Callie; Seay, Christopher; Sing, David K.; Benneke, Björn; Fraine, Jonathan D.; Kataria, Tiffany; Lewis, Nikole; Madhusudhan, Nikku; McCullough, Peter; Stevenson, Kevin B.; Wakeford, Hannah (2020), "Statistical Characterization of Hot Jupiter Atmospheres Using Spitzer's Secondary Eclipses", The Astronomical Journal, 159 (4): 137, arXiv: 1901.07040 , Bibcode:2020AJ....159..137G, doi: 10.3847/1538-3881/ab6cff , S2CID   119209434
  9. Wong, Ian; Shporer, Avi; Daylan, Tansu; Benneke, Björn; Fetherolf, Tara; Kane, Stephen R.; Ricker, George R.; Vanderspek, Roland; Latham, David W.; Winn, Joshua N.; Jenkins, Jon M.; Boyd, Patricia T.; Glidden, Ana; Goeke, Robert F.; Sha, Lizhou; Ting, Eric B.; Yahalomi, Daniel (2020), "Systematic phase curve study of known transiting systems from year one of the TESS mission", The Astronomical Journal, 160 (4): 155, arXiv: 2003.06407 , Bibcode:2020AJ....160..155W, doi: 10.3847/1538-3881/ababad , S2CID   212717799
  10. Mansfield, Megan; Wiser, Lindsey; Stevenson, Kevin B.; Smith, Peter; Line, Michael R.; Bean, Jacob L.; Fortney, Jonathan J.; Parmentier, Vivien; Kempton, Eliza M.-R.; Arcangeli, Jacob; Désert, Jean-Michel; Kilpatrick, Brian; Kreidberg, Laura; Malik, Matej (2022), "Confirmation of Water Absorption in the Thermal Emission Spectrum of the Hot Jupiter WASP-77Ab with HST/WFC3", The Astronomical Journal, 163 (6): 261, arXiv: 2203.01463 , Bibcode:2022AJ....163..261M, doi: 10.3847/1538-3881/ac658f , S2CID   247223194