Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Virgo |
Right ascension | 14h 12m 37.53311s[1] |
Declination | +04° 03′ 36.1166″[1] |
Apparent magnitude (V) | 11.76[2] |
Characteristics | |
Spectral type | K1V |
Astrometry | |
Radial velocity (Rv) | 14.10±0.39[1] km/s |
Proper motion (μ) | RA: 37.735 mas/yr[1] Dec.: -142.816 mas/yr[1] |
Parallax (π) | 6.9985 ± 0.0204 mas[1] |
Distance | 466 ± 1 ly (142.9 ± 0.4 pc) |
Details[3] | |
Mass | 0.81 M☉ |
Radius | 0.78 R☉ |
Temperature | 5079±88 K |
Metallicity | -0.04±0.08[4] |
Rotational velocity (v sin i) | 1.8 km/s |
Other designations | |
Database references | |
SIMBAD | data |
HAT-P-26 is a K-type main-sequence star about 466 light-years (143 parsecs) away. A survey in 2015 did not find any stellar companions in orbit around it,[5] although a red dwarf companion with a temperature 4000+100
−350 K is suspected on wide orbit.[6]
Nomenclature[edit]
The designation HAT-P-26 indicates that this was the 26th star found to have a planet by the HATNet Project.
In August 2022, this planetary system was included among 20 systems to be named by the third NameExoWorlds project.[7] The approved names, proposed by a team from Puerto Rico, were announced in June 2023. HAT-P-26 is named Guahayona and its planet is named Guataubá, after figures from Taíno mythology.[8]
Planetary system[edit]
In 2010 a transiting hot Neptune like planet was detected.[4] The transiting planet HAT-P-26b was detected by the HATNet Project using telescopes located in Hawaii and Arizona. The planet is likely formed by pebble accretion mechanism.[9]
The transmission spectrum of HAT-P-26b was taken in 2015, with the best fit favouring either a cloudless atmosphere or an atmosphere with a low-lying cloud deck.[10] The atmospheric composition of the planet was measured in 2019, and a water vapor volume fraction of 1.5+2.1
−0.9% was detected. HAT-P-26 is carbon depleted, with a C/O ratio constrained to less than 0.33. Also, the planet's atmosphere contains light metal hydrides.[11] The measured planetary temperature is equal to 563+58
−54 K.
In 2019, a transit timing variation analysis of HAT-P-26b indicated the possible presence of a second planet in the system on a wide, 1141-days orbit.[12]
In 2023, the atmosphere of the planet was confirmed to contain 12±2% steam at 590+20
−30K.[13]
Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
---|---|---|---|---|---|---|
b / Guataubá | >0.0585±0.00717 MJ | 0.0479±0.0006 | 4.234516±0.000015 | 0.124±0.060 | 88.6±0.9° | 0.5647±0.0517 RJ |
c (unconfirmed) | — | — | 1141 | — | — | — |
References[edit]
- ^ a b c d e 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 HAT-P-26 -- High proper-motion Star
- ^ D. Ehrenreich and J.-M. Désert, "Mass-loss rates for transiting exoplanets", A&A 529, A136 (2011)
- ^ a b Hartman, J. D.; Bakos, G. Á.; Kipping, D. M.; Torres, G.; Kovács, G.; Noyes, R. W.; Latham, D. W.; Howard, A. W.; Fischer, D. A.; Johnson, J. A.; Marcy, G. W.; Isaacson, H.; Quinn, S. N.; Buchhave, L. A.; Béky, B.; Sasselov, D. D.; Stefanik, R. P.; Esquerdo, G. A.; Everett, M.; Perumpilly, G.; Lázár, J.; Papp, I.; Sári, P. (2010), "HAT-P-26b: A LOW-DENSITY NEPTUNE-MASS PLANET TRANSITING A K STAR", The Astrophysical Journal, 728 (2): 138, arXiv:1010.1008, doi:10.1088/0004-637X/728/2/138, S2CID 119228956
- ^ 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
- ^ Piskorz, Danielle; Knutson, Heather A.; Ngo, Henry; Muirhead, Philip S.; Batygin, Konstantin; Crepp, Justin R.; Hinkley, Sasha; Morton, Timothy D. (2015), "Friends of Hot Jupiters. III. An Infrared Spectroscopic Search for Low-Mass Stellar Companions", The Astrophysical Journal, 814 (2): 148, arXiv:1510.08062, Bibcode:2015ApJ...814..148P, doi:10.1088/0004-637X/814/2/148, S2CID 11525988
- ^ "List of ExoWorlds 2022". nameexoworlds.iau.org. IAU. 8 August 2022. Retrieved 27 August 2022.
- ^ "2022 Approved Names". nameexoworlds.iau.org. IAU. Retrieved 7 June 2023.
- ^ Mohamad Ali-Dib, Gunjan Lakhlani, "Possible formation pathways for the low-density Neptune-mass planet HAT-P-26b"
- ^ Stevenson, Kevin B.; Bean, Jacob L.; Seifahrt, Andreas; Gilbert, Gregory J.; Line, Michael R.; Désert, Jean-Michel; Fortney, Jonathan J. (2015), "A SEARCH FOR WATER IN THE ATMOSPHERE OF HAT-P-26b USING LDSS-3C", The Astrophysical Journal, 817 (2): 141, arXiv:1511.08226, doi:10.3847/0004-637X/817/2/141, S2CID 118394486
- ^ MacDonald, Ryan J.; Madhusudhan, Nikku (2019), "The Metal-Rich Atmosphere of the Neptune HAT-P-26b", Monthly Notices of the Royal Astronomical Society, 486: 1292–1315, arXiv:1903.09151, doi:10.1093/mnras/stz789, S2CID 85459516
- ^ a b von Essen, C.; Wedemeyer, S.; Sosa, M. S.; Hjorth, M.; Parkash, V.; Freudenthal, J.; Mallonn, M.; Miculán, R. G.; Zibecchi, L.; Cellone, S.; Torres, A. F. (2019), "Indications for transit timing variations in the exo-Neptune HAT-P-26b", Astronomy & Astrophysics, 628: A116, arXiv:1904.06360, Bibcode:2019A&A...628A.116V, doi:10.1051/0004-6361/201731966, S2CID 118674293
- ^ A-thano, Napaporn; Awiphan, Supachai; Jiang, Ing-Guey; Kerins, Eamonn; Priyadarshi, Akshay; McDonald, Iain; Joshi, Yogesh C.; Chulikorn, Thansuda; Hayes, Joshua J. C.; Charles, Stephen; Huang, Chung-Kai; Rattanamala, Ronnakrit; Yeh, Li-Chin; Vik S Dhillon (2023), "Revisiting the Transit Timing and Atmosphere Characterization of the Neptune-mass Planet HAT-P-26 b", The Astronomical Journal, 166 (6): 223, arXiv:2303.03610, Bibcode:2023AJ....166..223A, doi:10.3847/1538-3881/acfeea
- ^ Planet HAT-P-26 b on exoplanet.eu
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.
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