HAT-P-41 is a binary star system. Its primary is a F-type main-sequence star. Its surface temperature is 6390±100 K.[4] 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.[4]
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Aquila |
| Right ascension | 19h 49m 17.4400s[1] |
| Declination | 04° 40′ 20.7836″[1] |
| Apparent magnitude (V) | 11.36 |
| Characteristics | |
| HAT-P-41 | |
| Evolutionary stage | main-sequence star |
| Spectral type | F9V[2] |
| HAT-P-41B | |
| Spectral type | K9-M0[2] |
| Astrometry | |
| Radial velocity (Rv) | 33.2±0.5[3] km/s |
| Proper motion (μ) | RA: −3.177[3] mas/yr Dec.: −6.570[3] mas/yr |
| Parallax (π) | 2.8477 ± 0.0176 mas[3] |
| Distance | 1,145 ± 7 ly (351 ± 2 pc) |
| Position (relative to HAT-P-41)[2] | |
| Component | HAT-P-41B |
| Epoch of observation | 2013 |
| Angular distance | 3.619±0.005″ |
| Position angle | 184.1±0.2° |
| Projected separation | 1270 AU |
| Details[4] | |
| Mass | 1.418±0.047 M☉ |
| Radius | 1.683+0.058 −0.036 R☉ |
| Temperature | 6390±100 K |
| Metallicity [Fe/H] | 0.21±0.10 dex |
| Rotational velocity (v sin i) | 19.60±0.50 km/s |
| Age | 2.2±0.4 Gyr |
| Other designations | |
| HAT-P-41: Gaia DR2 4290415081653653632, Gaia EDR3 4290415081653653632 | |
| HAT-P-41B: Gaia DR2 4290415081653653376, Gaia EDR3 4290415081653653376 | |
| Database references | |
| SIMBAD | data |
| Hat-P-41b | |
The candidate stellar companion was detected simultaneously with the planet discovery in 2012.[5] A multiplicity survey in 2015 did confirm a dim stellar companion of later-K to early-M spectral class, with the probability of being a background star of 14%.[2] By 2020, it was concluded the candidate companion star is probably gravitationally bound.[6]
Planetary system
editIn 2012, one planet, named HAT-P-41b, was discovered on a tight, circular orbit around the primary star.[5]
The planetary orbit is mildly misaligned with the equatorial plane of the star, misalignment angle equal to −22.1+0.8
−6.0 degrees.[7]
The transmission spectrum of HAT-P-41b taken in 2020 has resulted in contradictory interpretations. One team has concluded the planetary atmosphere is metal-rich, with clear water signatures and absorption bands from sodium, aluminum, titanium and vanadium compounds.[8] Another team has interpreted the results as arising from a dense hydrogen atmosphere without detectable heavy elements, but with significant ionization.[9] The atmosphere also appears to contain significant cloud and hazes.[10] Neither heavy element compounds nor H− ion opacity were found in 2022 study.[11]
The planetary equilibrium temperature is within 1700-1950 K,[9] and the dayside temperature has been measured at 1622±125 K.[12]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 0.795+0.056 −0.091 MJ |
0.04258+0.00047 −0.00048 |
2.694047±0.000004 | <0.22 | 87.7±1.0° | 1.685+0.076 −0.051 RJ |
References
edit- ^ a b c "HAT-P-41". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-01-21.
- ^ a b c d Wöllert, Maria; Brandner, Wolfgang; Bergfors, Carolina; Henning, Thomas (2015), "A Lucky Imaging search for stellar companions to transiting planet host stars", Astronomy & Astrophysics, 575: A23, arXiv:1507.01938, Bibcode:2015A&A...575A..23W, doi:10.1051/0004-6361/201424091, S2CID 119250579
- ^ a b c d Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ a b c d Bonomo, A. S.; Desidera, S.; Benatti, S.; Borsa, F.; Crespi, S.; Damasso, M.; Lanza, A. F.; Sozzetti, A.; Lodato, G.; Marzari, F.; Boccato, C.; Claudi, R. U.; Cosentino, R.; Covino, E.; Gratton, R.; Maggio, A.; Micela, G.; Molinari, E.; Pagano, I.; Piotto, G.; Poretti, E.; Smareglia, R.; Affer, L.; Biazzo, K.; Bignamini, A.; Esposito, M.; Giacobbe, P.; Hébrard, G.; Malavolta, L.; et al. (2017), "The GAPS Programme with HARPS-N at TNG", Astronomy & Astrophysics, 602: A107, arXiv:1704.00373, Bibcode:2017A&A...602A.107B, doi:10.1051/0004-6361/201629882, S2CID 118923163
- ^ a b Hartman, J. D.; et al. (2012), "HAT-P-39b–HAT-P-41b: Three Highly Inflated Transiting Hot Jupiters", The Astronomical Journal, 144 (5): 139, arXiv:1207.3344, Bibcode:2012AJ....144..139H, doi:10.1088/0004-6256/144/5/139, S2CID 118457589
- ^ Bohn, A. J.; Southworth, J.; Ginski, C.; Kenworthy, M. A.; Maxted, P. F. L.; Evans, D. F. (2020), "A multiplicity study of transiting exoplanet host stars", Astronomy & Astrophysics, 635: A73, arXiv:2001.08224, Bibcode:2020A&A...635A..73B, doi:10.1051/0004-6361/201937127, S2CID 210861118
- ^ Johnson, Marshall C.; Cochran, William D.; Addison, Brett C.; Tinney, Chris G.; Wright, Duncan J. (2017), "Spin–Orbit Misalignments of Three Jovian Planets via Doppler Tomography", The Astronomical Journal, 154 (4): 137, arXiv:1708.01291, Bibcode:2017AJ....154..137J, doi:10.3847/1538-3881/aa8462, S2CID 119487498
- ^ Sheppard, Kyle B.; et al. (2021). "The Hubble PanCET Program: A Metal-rich Atmosphere for the Inflated Hot Jupiter HAT-P-41b". The Astronomical Journal. 161 (2): 51. arXiv:2010.09659. Bibcode:2021AJ....161...51S. doi:10.3847/1538-3881/abc8f4. S2CID 224710738.
- ^ a b Lewis, N. K.; et al. (2020), "Into the UV: The Atmosphere of the Hot Jupiter HAT-P-41b Revealed", The Astrophysical Journal, 902 (1): L19, arXiv:2010.08551, Bibcode:2020ApJ...902L..19L, doi:10.3847/2041-8213/abb77f, S2CID 224706001
- ^ Wakeford, H. R.; Sing, D. K.; Stevenson, K. B.; Lewis, N. K.; Pirzkal, N.; Wilson, T. J.; Goyal, J.; Kataria, T.; Mikal-Evans, T.; Nikolov, N.; Spake, J. (2020), "Into the UV: A Precise Transmission Spectrum of HAT-P-41b Using Hubble's WFC3/UVIS G280 Grism", The Astronomical Journal, 159 (5): 204, arXiv:2003.00536, Bibcode:2020AJ....159..204W, doi:10.3847/1538-3881/ab7b78, S2CID 211677682
- ^ Fu, Guangwei; Sing, David K.; Deming, Drake; Sheppard, Kyle; Wakeford, H. R.; Mikal-Evans, Thomas; Alam, Munazza K.; Dos Santos, Leonardo A.; López-Morales, Mercedes; Lothringer, Joshua D. (2022), "The Hubble PanCET Program: Emission Spectrum of Hot Jupiter HAT-P-41b", The Astronomical Journal, 163 (4): 190, arXiv:2202.12314, Bibcode:2022AJ....163..190F, doi:10.3847/1538-3881/ac58fc, S2CID 247154998
- ^ 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