| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Cetus |
| Right ascension | 01h 52m 50.534416s[1] |
| Declination | −19° 30′ 25.108238″[1] |
| Apparent magnitude (V) | 7.51[2] |
| Characteristics | |
| Spectral type | G0V[3] |
| B−V color index | 0.607±0.015[2] |
| Astrometry | |
| Radial velocity (Rv) | −7.53±0.13[1] km/s |
| Proper motion (μ) | RA: 22.039±0.022[1] mas/yr Dec.: −97.904±0.016[1] mas/yr |
| Parallax (π) | 19.5342 ± 0.0221 mas[1] |
| Distance | 167.0 ± 0.2 ly (51.19 ± 0.06 pc) |
| Absolute magnitude (MV) | 3.94[2] |
| Details[4] | |
| Mass | 1.12±0.02 M☉ |
| Radius | 1.06±0.01 R☉ |
| Luminosity | 1.17±0.01 L☉ |
| Surface gravity (log g) | 4.43±0.02 cgs |
| Temperature | 5,833±28 K |
| Metallicity [Fe/H] | 0.29±0.03[5] dex |
| Rotational velocity (v sin i) | 5.01[6] km/s |
| Age | 1.6±0.9 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
HD 11506 is a star in the equatorial constellation of Cetus. It has a yellow hue and can be viewed with a small telescope but is too faint to be visible to the naked eye, having an apparent visual magnitude of 7.51.[2] The distance to this object is 167 light years based on parallax, but it is drifting closer to the Sun with a radial velocity of −7.5 km/s.[1] It has an absolute magnitude of 3.94.[2]
This object is an ordinary G-type main-sequence star with a stellar classification of G0V,[3] which indicates it is generating energy via hydrogen fusion at its core. It is around 1.6[4] billion years old and is spinning with a projected rotational velocity of 5 km/s.[6] The star has 112% of the mass of the Sun and 106% of the Sun's radius. The spectrum shows a higher than solar abundance of elements other than hydrogen and helium – what astronomers term the metallicity.[5] The star is radiating 117% of the Sun's luminosity from its photosphere at an effective temperature of 5,833 K.[4]
Planetary system
[edit]The superjovian planet HD 11506 b was discovered orbiting the star by the N2K Consortium in 2007 using the doppler spectroscopy method.[3] In 2009, a second planet discovery was claimed based on Bayesian analysis of the original data.[8] However, in 2015 additional radial velocity measurements showed that the planetary parameters were significantly different than those determined by Bayesian analysis. An additional linear trend in the radial velocities indicates a stellar or planetary companion on a long term orbit.[5] In 2022, the presence of a third planet with an orbital period of 40 years was confirmed, and the mass and inclination of both planet b and the new planet d were measured via astrometry.[9]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| c | ≥0.408±0.057 MJ | 0.774±0.038 | 223.41±0.32 | 0.193±0.038 | — | — |
| b | 4.880+1.986 −0.333 MJ |
2.800+0.123 −0.136 |
1,613.7+4.3 −4.5 |
0.391±0.010 | 112.598+23.304 −52.700° |
— |
| d | 7.383+2.015 −1.085 MJ |
12.235+1.571 −1.762 |
14,723.6+2,801.3 −2,735.0 |
0.061+0.028 −0.022 |
82.004+25.098 −21.421° |
— |
References
[edit]- ^ a b c d e f g 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 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
- ^ a b c Fischer, Debra A.; et al. (2007). "Five Intermediate-Period Planets from the N2K Sample". The Astrophysical Journal. 669 (2): 1336–1344. arXiv:0704.1191. Bibcode:2007ApJ...669.1336F. doi:10.1086/521869. S2CID 7774321.
- ^ a b c Bonfanti, A.; et al. (2015). "Revising the ages of planet-hosting stars". Astronomy and Astrophysics. 575. A18. arXiv:1411.4302. Bibcode:2015A&A...575A..18B. doi:10.1051/0004-6361/201424951. S2CID 54555839.
- ^ a b c Giguere, Matthew J.; et al. (2015). "Newly Discovered Planets Orbiting HD 5319, HD 11506, HD 75784 and HD 10442 from the N2K Consortium". The Astrophysical Journal. 799 (1). 89. arXiv:1411.5374. Bibcode:2015ApJ...799...89G. doi:10.1088/0004-637X/799/1/89. S2CID 56121568.
- ^ a b Delgado Mena, E.; et al. (April 2015). "Li abundances in F stars: planets, rotation, and Galactic evolution". Astronomy & Astrophysics. 576: 24. arXiv:1412.4618. Bibcode:2015A&A...576A..69D. doi:10.1051/0004-6361/201425433. S2CID 56051637. A69.
- ^ "HD 11506". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-11-10.
- ^ Tuomi, M.; Kotiranta, S. (2009). "Bayesian analysis of the radial velocities of HD 11506 reveals another planetary companion". Astronomy and Astrophysics. 496 (2): L13–L16. arXiv:0902.2997. Bibcode:2009A&A...496L..13T. doi:10.1051/0004-6361/200811531. S2CID 16414890.
- ^ a b Feng, Fabo; Butler, R. Paul; et al. (August 2022). "3D Selection of 167 Substellar Companions to Nearby Stars". The Astrophysical Journal Supplement Series. 262 (21): 21. arXiv:2208.12720. Bibcode:2022ApJS..262...21F. doi:10.3847/1538-4365/ac7e57. S2CID 251864022.
- ^ Ment, Kristo; et al. (2018). "Radial Velocities from the N2K Project: Six New Cold Gas Giant Planets Orbiting HD 55696, HD 98736, HD 148164, HD 203473, and HD 211810". The Astronomical Journal. 156 (5). 213. arXiv:1809.01228. Bibcode:2018AJ....156..213M. doi:10.3847/1538-3881/aae1f5. S2CID 119243619.
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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