| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Eridanus |
| Right ascension | 05h 04m 19.6323s[1] |
| Declination | −06° 13′ 47.378″[1] |
| Apparent magnitude (V) | 10.94 |
| Characteristics | |
| Spectral type | G0V |
| Astrometry | |
| Radial velocity (Rv) | 16.96[2] km/s |
| Proper motion (μ) | RA: 20.758(15) mas/yr[1] Dec.: 10.963(11) mas/yr[1] |
| Parallax (π) | 4.9411 ± 0.0160 mas[1] |
| Distance | 660 ± 2 ly (202.4 ± 0.7 pc) |
| Details[3][4][5] | |
| Mass | 1.06±0.08 M☉ |
| Radius | 1.09±0.02 R☉ |
| Surface gravity (log g) | 4.39±0.02 cgs |
| Temperature | 6072±62 K |
| Metallicity [Fe/H] | 0.01±0.05 dex |
| Rotational velocity (v sin i) | 2.4±0.6 km/s |
| Age | 5.0±1.2 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
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.[6]
The star has no detectable starspot activity.[4] An imaging survey in 2015 found no detectable stellar companions,[7] although a spectroscopic survey in 2016 yielded a suspected red dwarf companion with a temperature of 3800±1100 K.[8]
Planetary system
[edit]In 2011 a transiting hot Jupiter planet b was detected. The planet's equilibrium temperature is 1450±20 K.[4]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 0.765±0.029 MJ | 0.04360±0.00020 | 3.1615691±0.0000003 | 0 | 87.95±0.33° | 1.349±0.022 RJ |
References
[edit]- ^ 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 "WASP-35". SIMBAD. Centre de données astronomiques de Strasbourg.
- ^ Mortier, A.; Santos, N. C.; Sousa, S. G.; Fernandes, J. M.; Adibekyan, V. Zh.; Delgado Mena, E.; Montalto, M.; Israelian, G. (2013), "New and updated stellar parameters for 90 transit hosts The effect of the surface gravity", Astronomy and Astrophysics, 558: A106, arXiv:1309.1998, Bibcode:2013A&A...558A.106M, doi:10.1051/0004-6361/201322240, S2CID 118750676
- ^ a b c Enoch, B.; Anderson, D. R.; Barros, S. C. C.; Brown, D. J. A.; Cameron, A. Collier; Faedi, F.; Gillon, M.; Hébrard, G.; Lister, T. A.; Queloz, D.; Santerne, A.; Smalley, B.; Street, R. A.; Triaud, A. H. M. J.; West, R. G.; Bouchy, F.; Bento, J.; Butters, O.; Fossati, L.; Haswell, C. A.; Hellier, C.; Holmes, S.; Jehen, E.; Lendl, M.; Maxted, P. F. L.; McCormac, J.; Miller, G. R. M.; Moulds, V.; Moutou, C.; et al. (2011), "WASP-35b, WASP-48b, AND HAT-P-30b/WASP-51b: TWO NEW PLANETS AND AN INDEPENDENT DISCOVERY OF a HAT PLANET", The Astronomical Journal, 142 (3): 86, arXiv:1104.2827, Bibcode:2011AJ....142...86E, doi:10.1088/0004-6256/142/3/86, S2CID 63996398
- ^ 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@TNG XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets", Astronomy & Astrophysics, A107: 602, arXiv:1704.00373, Bibcode:2017A&A...602A.107B, doi:10.1051/0004-6361/201629882, S2CID 118923163
- ^ Mortier, A.; Sousa, S. G.; Adibekyan, V. Zh.; Brandão, I. M.; Santos, N. C. (2014), "Correcting the spectroscopic surface gravity using transits and asteroseismology. No significant effect on temperatures or metallicities with ARES and MOOG in local thermodynamic equilibrium", Astronomy and Astrophysics, 572: A95, arXiv:1410.1310, Bibcode:2014A&A...572A..95M, doi:10.1051/0004-6361/201424537, S2CID 73621824
- ^ Wöllert, Maria; Brandner, Wolfgang (2015), "A Lucky Imaging search for stellar sources near 74 transit hosts", Astronomy & Astrophysics, 579: A129, arXiv:1506.05456, Bibcode:2015A&A...579A.129W, doi:10.1051/0004-6361/201526525, S2CID 118903879
- ^ Evans, D. F.; Southworth, J.; Maxted, P. F. L.; Skottfelt, J.; Hundertmark, M.; Jørgensen, U. G.; Dominik, M.; Alsubai, K. A.; Andersen, M. I.; Bozza, V.; Bramich, D. M.; Burgdorf, M. J.; Ciceri, S.; d'Ago, G.; Figuera Jaimes, R.; Gu, S.-H.; Haugbølle, T.; Hinse, T. C.; Juncher, D.; Kains, N.; Kerins, E.; Korhonen, H.; Kuffmeier, M.; Mancini, L.; Peixinho, N.; Popovas, A.; Rabus, M.; Rahvar, S.; Schmidt, R. W.; et al. (2016), "High-resolution Imaging of Transiting Extrasolar Planetary systems (HITEP). I. Lucky imaging observations of 101 systems in the southern hemisphere", Astronomy & Astrophysics, 589: A58, arXiv:1603.03274, Bibcode:2016A&A...589A..58E, doi:10.1051/0004-6361/201527970, S2CID 14215845
- ^ Bai, Lu; Gu, Shenghong; Wang, Xiaobin; Sun, Leilei; Kwok, Chi-Tai; Hui, Ho-Keung (2022), "WASP-35 and HAT-P-30/WASP-51: Reanalysis using TESS and Ground-based Transit Photometry", The Astronomical Journal, 163 (5): 208, arXiv:2203.02866, Bibcode:2022AJ....163..208B, doi:10.3847/1538-3881/ac5b6a, S2CID 247292453
Well, that’s interesting to know that Psilotum nudum are known as whisk ferns. Psilotum nudum is the commoner species of the two. While the P. flaccidum is a rare species and is found in the tropical islands. Both the species are usually epiphytic in habit and grow upon tree ferns. These species may also be terrestrial and grow in humus or in the crevices of the rocks.
View the detailed Guide of Psilotum nudum: Detailed Study Of Psilotum Nudum (Whisk Fern), Classification, Anatomy, Reproduction