HD 147506

Last updated
HD 147506 / Hunor
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Hercules [1]
Right ascension 16h 20m 36.3576s [2]
Declination +41° 02′ 53.107″ [2]
Apparent magnitude  (V)+8.71 [3]
Characteristics
Spectral type F8V [3]
Variable type planetary transit, [4] planet-induced stellar pulsations [5]
Astrometry
Radial velocity (Rv)−20.47±0.30 [2]  km/s
Proper motion (μ)RA: −10.078(12)  mas/yr [2]
Dec.: −29.057(15)  mas/yr [2]
Parallax (π)7.7811 ± 0.0118  mas [2]
Distance 419.2 ± 0.6  ly
(128.5 ± 0.2  pc)
Absolute magnitude  (MV)+3.31 [6]
Details
Mass 1.360±0.040 [7]   M☉
Radius 1.640+0.090
−0.080 [7]   R☉
Luminosity 4.3 [2]   L☉
Surface gravity (log g)4.14±0.04 [8]   cgs
Temperature 6,290±60 [7]   K
Metallicity [Fe/H]0.140±0.080 [7]   dex
Rotational velocity (v sin i)20.80±0.30 [7]  km/s
Age 2.60±0.50 [7]   Gyr
Other designations
HAT-P-2, BD+41°2693, HD  147506, HIP  80076, SAO  46035 [3]
Database references
SIMBAD data

HD 147506, also known as HAT-P-2 and formally named Hunor, is a magnitude 8.7 F8 dwarf star that is somewhat larger and hotter than the Sun. The star is approximately 419 light-years (128 parsecs ) from Earth and is positioned near the keystone of Hercules. [3] It is estimated to be 2 to 3 billion years old, towards the end of its main sequence life. [2] There is one known transiting exoplanet, and a second planet not observed to transit. [9]

Contents

Nomenclature

The designation HD 147506 comes from the Henry Draper Catalogue. When the star was found to have a planet by the HATNet Project, it was assigned the designation HAT-P-2, indicating that it was the second star found to have a planet by this project. [4]

The star HAT-P-2 has the proper name Hunor. The name was selected in the NameExoWorlds campaign by Hungary, during the 100th anniversary of the IAU. Hunor was a legendary ancestor of the Huns and the Hungarian nation, and brother of Magor (name of the planet HAT-P-2b). [10]

Variability

In addition to being a planetary transit variable, there are also stellar pulsations induced by the planet. This is the first known instance of a planet inducing pulsations in its host star. The amplitude is very small at approximately 40 parts per million. These pulsations correspond to exact harmonics of the planet's orbital frequency, indicating they are of a tidal origin. [5]

Planetary system

Orbiting the star is HAT-P-2b, later named Magor, which was at the time of its discovery the most massive transiting exoplanet. [4] At around 9 times the mass of Jupiter and an estimated surface temperature of ~900 kelvins, on a 5.6 day orbit, this planet is unlike any previously discovered transiting planet. The planet has a large mass (nine times the mass of Jupiter), and a surface gravity 25 times that exerted by the Earth. Its orbital eccentricity is very large (e = 0.5). Since tidal forces should have reduced the orbital eccentricity of this planet, it was speculated that another massive planet found outside the orbit of HAT-P-2b is in orbital resonance with HAT-P-2b. [11] [6]

The planet was discovered by the HATNet Project, and the researchers there found the planet to be 10-20% larger than Jupiter. This discovery is important as it provides further support for the existing theory of planetary structure. [12]

Additional measurements taken over six years show a long-term linear trend in the radial velocity data consistent with a companion of 15 Jupiter masses or greater. Adaptive optics images were taken at the Keck telescope, and when combined with the radial velocity data show the maximum mass of the companion is that of an M dwarf star. [13] In 2023 the presence of an outer companion, HAT-P-2c, was confirmed, and its mass found to be planetary at around 11 times that of Jupiter. [9]

The HD 147506 planetary system [7] [9]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b / Magor 8.70+0.19
−0.20  MJ 		0.06880+0.00065
−0.00070		5.6334754(26)0.50833+0.00082
−0.00075		86.72+1.1
−0.87 ° 		1.157+0.073
−0.063  RJ
c10.7+5.2
−2.2  MJ 		—8500+2600
−1500		0.37+0.13
−0.12		90±16 ° —

See also

Related Research Articles

<span class="mw-page-title-main">HAT-P-1b</span> Hot Jupiter orbiting HAT-P-1

HAT-P-1b is an extrasolar planet orbiting the Sun-like star HAT-P-1, also known as ADS 16402 B. HAT-P-1 is the dimmer component of the ADS 16402 binary star system. It is located roughly 521 light years away from Earth in the constellation Lacerta. HAT-P-1b is among the least dense of any of the known extrasolar planets.

<span class="mw-page-title-main">HAT-P-2b</span> Extrasolar planet

HAT-P-2b is an extrasolar planet detected by the HATNet Project in May 2007. It orbits a class F star HAT-P-2,, located about 420 light-years away in the constellation Hercules.

The Hungarian Automated Telescope Network (HATNet) project is a network of six small fully automated "HAT" telescopes. The scientific goal of the project is to detect and characterize extrasolar planets using the transit method. This network is used also to find and follow bright variable stars. The network is maintained by the Center for Astrophysics | Harvard & Smithsonian.

<span class="mw-page-title-main">HAT-P-4b</span> Exoplanet orbiting HAT-P-4b in the constellation Boötes

HAT-P-4b is a confirmed extrasolar planet orbiting the star HAT-P-4 over 1000 light years away in Boötes constellation. It was discovered by transit on October 2, 2007, which looks for slight dimming of stars caused by planets that passed in front of them. It is the fourth planet discovered by the HATNet Project. It is also called BD+36 2593b, TYC 2569-01599-1b, 2MASS J15195792+3613467b, SAO 64638b.

WASP-11/HAT-P-10 is a binary star. It is a primary main-sequence orange dwarf star. Secondary is M-dwarf with a projected separation of 42 AU. The system is located about 424 light-years away in the constellation Aries.

HD 210277 b is an extrasolar planet orbiting the star HD 210277. It was discovered in September 1998 by the California and Carnegie Planet Search team using the highly successful radial velocity method. The planet is at least 24% more massive than Jupiter. The mean distance of the planet from the star is slightly more than Earth's distance from the Sun. However, the orbit is very eccentric, so at periastron this distance is almost halved, and at apastron it is as distant as Mars is from the Sun.

<span class="mw-page-title-main">HD 17156 b</span> Extrasolar planet in the constellation of Cassiopeia

HD 17156 b, named Mulchatna by the IAU, is an extrasolar planet approximately 255 light-years away in the constellation of Cassiopeia. The planet was discovered orbiting the yellow subgiant star HD 17156 in April 2007. The planet is classified as a relatively cool hot Jupiter planet slightly smaller than Jupiter but slightly larger than Saturn. This highly-eccentric three-week orbit takes it approximately 0.0523 AU of the star at periastron before swinging out to approximately 0.2665 AU at apastron. Its eccentricity is about the same as 16 Cygni Bb, a so-called "eccentric Jupiter". Until 2009, HD 17156 b was the transiting planet with the longest orbital period.

XO-2 is a binary star system about 490 light-years away in the constellation Lynx. It consists of two components, XO-2N and XO-2S, both of which host planetary systems.

<span class="mw-page-title-main">HAT-P-8b</span> Extrasolar planet in the constellation Pegasus

HAT-P-8b is an extrasolar planet located approximately 720 light years away in the constellation of Pegasus, orbiting the 10th magnitude star GSC 02757-01152. This planet was discovered by transit on December 5, 2008. Despite the designation as HAT-P-8b, it is the 11th planet discovered by the HATNet Project. The mass of the planet is 50% more than Jupiter while the radius is also 50% more than Jupiter. The mass of this planet is exact since the inclination of the orbit is known, typical for transiting planets. This is a so-called “hot Jupiter” because this Jupiter-like gas giant planet orbits in a really close torch orbit around the star, making this planet extremely hot. The distance from the star is roughly 20 times smaller than that of Earth from the Sun, which places the planet roughly 8 times closer to its star than Mercury is from the Sun. The “year” on this planet lasts only 3 days, 1 hour, 49 minutes, and 54 seconds, compared with Earth's 365 days, 6 hours, 9 minutes, and 10 seconds in a sidereal year.

HAT-P-8 is a magnitude 10 star located 700 light-years away in Pegasus. It is a F-type star about 28% more massive than the Sun. Two red dwarf companions have been detected around HAT-P-8. The first has a spectral type of M5V and has a mass of 0.22 M☉. The second is even less massive, at 0.18 M☉, and its spectral type is M6V.

HAT-P-17 is a K-type main-sequence star about 92.6 parsecs (302 ly) away. It has a mass of about 0.857 ± 0.039 M☉. It is the host of two planets, HAT-P-17b and HAT-P-17c, both discovered in 2010. A search for a binary companion star using adaptive optics at the MMT Observatory was negative. A candidate companion was detected by a spectroscopic search of high-resolution K band infrared spectra taken at the Keck observatory.

HD 146389, is a star with a yellow-white hue in the northern constellation of Hercules. The star was given the formal name Irena by the International Astronomical Union in January 2020. It is invisible to the naked eye with an apparent visual magnitude of 9.4 The star is located at a distance of approximately 446 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −9 km/s. The star is known to host one exoplanet, designated WASP-38b or formally named 'Iztok'.

HAT-P-26 is a K-type main-sequence star about 466 light-years away. A survey in 2015 did not find any stellar companions in orbit around it, although a red dwarf companion with a temperature 4000+100
−350 K is suspected on wide orbit.

References

  1. ↑ Roman, Nancy G. (1987). "Identification of a Constellation From a Position". Publications of the Astronomical Society of the Pacific. 99 (617): 695–699. Bibcode:1987PASP...99..695R. doi: 10.1086/132034 . Vizier query form
  2. 1 2 3 4 5 6 7 8 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.
  3. 1 2 3 4 "HD 147506". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2009-04-24.
  4. 1 2 3 Bakos, G. Á.; et al. (2007). "HD 147506b: A Supermassive Planet in an Eccentric Orbit Transiting a Bright Star". The Astrophysical Journal. 670 (1): 826–832. arXiv: 0705.0126 . Bibcode: 2007ApJ...670..826B . doi: 10.1086/521866 . S2CID   18286425.
  5. 1 2 Wit, Julien de; et al. (2017). "Planet-induced Stellar Pulsations in HAT-P-2's Eccentric System". The Astrophysical Journal Letters. 836 (2) L17. arXiv: 1702.03797 . Bibcode: 2017ApJ...836L..17D . doi: 10.3847/2041-8213/836/2/L17 . S2CID   45906585.
  6. 1 2 Pál, András; et al. (2010). "Refined stellar, orbital and planetary parameters of the eccentric HAT-P-2 planetary system". Monthly Notices of the Royal Astronomical Society. 401 (4): 2665–2674. arXiv: 0908.1705 . Bibcode: 2010MNRAS.401.2665P . doi: 10.1111/j.1365-2966.2009.15849.x .
  7. 1 2 3 4 5 6 7 Bonomo, A. S.; et al. (2017). "The GAPS Programme with HARPS-N at TNG . XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets". Astronomy and Astrophysics. 602 A107. arXiv: 1704.00373 . Bibcode: 2017A&A...602A.107B . doi: 10.1051/0004-6361/201629882 . S2CID   118923163.
  8. ↑ Torres, Guillermo; et al. (2012). "Improved Spectroscopic Parameters for Transiting Planet Hosts". The Astrophysical Journal. 757 (2) 161. arXiv: 1208.1268 . Bibcode: 2012ApJ...757..161T . doi: 10.1088/0004-637X/757/2/161 .
  9. 1 2 3 de Beurs, Zoë L.; et al. (October 2023). "Revisiting Orbital Evolution in HAT-P-2 b and Confirmation of HAT-P-2 c". The Astronomical Journal. 166 (4) 136. arXiv: 2309.03256 . Bibcode: 2023AJ....166..136D . doi: 10.3847/1538-3881/acedf1 .
  10. ↑ "Approved names". NameExoworlds. Retrieved 2020-01-02.
  11. ↑ Alan MacRobert, “New Worlds roundup,” Sky and Telescope, August 2007, pg 15.
  12. ↑ Systemic Planetary Simulation
  13. ↑ Lewis, Nikole K.; et al. (2013). "Orbital Phase Variations of the Eccentric Giant Planet HAT-P-2b". The Astrophysical Journal. 766 (2) 95. arXiv: 1302.5084 . Bibcode: 2013ApJ...766...95L . doi: 10.1088/0004-637X/766/2/95 .
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