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Coordinates: Sky map 04h 24m 59.5348s, +39° 27′ 38.3124″
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{{short description|Star in the constellation Perseus}}
{{short description|Star in the constellation Perseus}}
{{Starbox begin
{{Starbox begin
| name = HAT-P-15
| name = HAT-P-15 / Berehynia


}}
}}
{{Starbox observe
{{Starbox observe
| epoch = J2000
| epoch = J2000
⚫
| ra = {{RA|04|24|59.5348}}<ref name=simbad/>
⚫
| dec = {{DEC|+39|27|38.3124}}<ref name=simbad/>
| constell = [[Perseus (constellation)|Perseus]]
| constell = [[Perseus (constellation)|Perseus]]
⚫
| ra = {{RA|04|24|59.5350}}<ref name="Gaia DR3"/>
⚫
| dec = {{DEC|+39|27|38.313}}<ref name="Gaia DR3"/>
| appmag_v = 12.41
| appmag_v = 12.41
}}
}}
{{Starbox character
{{Starbox character
| class = G5V
| class = G5V
| variable = [[Variable star#Planetary transits|planetary transit]]<ref name=Kovacs2010/>
}}
}}
{{Starbox astrometry
{{Starbox astrometry
| radial_v = 31.21
| radial_v = 31.21
| prop_mo_ra = 14.403
| prop_mo_ra = {{val|14.233|(21)}}
| prop_mo_dec = -9.377
| prop_mo_dec = {{val|−9.407|(15)}}
| pm_footnote = <ref name="Gaia DR3"/>
| parallax = 5.1664
| p_error = 0.0544
| parallax = 5.1856
| p_error = 0.0166
| parallax_footnote = <ref name=simbad/>
| parallax_footnote = <ref name="Gaia DR3"/>
}}
}}
{{Starbox detail
{{Starbox detail
| source = <ref name=Teske2019>{{citation|arxiv=1912.00255|title=Do Metal-Rich Stars Make Metal-Rich Planets? New Insights on Giant Planet Formation from Host Star Abundances|year=2019|doi=10.3847/1538-3881/ab4f79|last1=Teske|first1=Johanna K.|last2=Thorngren|first2=Daniel|last3=Fortney|first3=Jonathan J.|last4=Hinkel|first4=Natalie|last5=Brewer|first5=John M.|journal=The Astronomical Journal|volume=158|issue=6|page=239|bibcode=2019AJ....158..239T|s2cid=208527082}}</ref>
| source = <ref name=Teske2019>{{citation|arxiv=1912.00255|title=Do Metal-Rich Stars Make Metal-Rich Planets? New Insights on Giant Planet Formation from Host Star Abundances|year=2019|doi=10.3847/1538-3881/ab4f79|last1=Teske|first1=Johanna K.|last2=Thorngren|first2=Daniel|last3=Fortney|first3=Jonathan J.|last4=Hinkel|first4=Natalie|last5=Brewer|first5=John M.|journal=The Astronomical Journal|volume=158|issue=6|page=239|bibcode=2019AJ....158..239T|s2cid=208527082 |doi-access=free }}</ref>
| mass = 1.013{{±|0.043}}
| mass = 1.013{{±|0.043}}
| radius = 1.080{{±|0.039}}
| radius = 1.080{{±|0.039}}
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}}
}}
{{Starbox catalog
{{Starbox catalog
| names = {{odlist|TYC=2883-1687-1|GSC=02883-01687|2MASS=J04245952+3927382|Gaia DR2=179498266829041664}}<ref name=simbad/>
| names = {{odlist | name=Berehynia | 2MASS=J04245952+3927382 | Gaia DR3=179498266829041664 | GSC=02883-01687 | TYC=2883-1687-1 }}<ref name=simbad/>
}}
}}
{{Starbox reference
{{Starbox reference
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The spectroscopic survey in 2015 have failed to find any stellar companions to it,<ref>{{citation|arxiv=1510.08062|title=Friends of Hot Jupiters III: An Infrared Spectroscopic Search for Low-Mass Stellar Companions|year=2015|doi=10.1088/0004-637X/814/2/148|last1=Piskorz|first1=Danielle|last2=Knutson|first2=Heather A.|last3=Ngo|first3=Henry|last4=Muirhead|first4=Philip S.|last5=Batygin|first5=Konstantin|last6=Crepp|first6=Justin R.|last7=Hinkley|first7=Sasha|last8=Morton|first8=Timothy D.|journal=The Astrophysical Journal|volume=814|issue=2|page=148|bibcode=2015ApJ...814..148P|s2cid=11525988}}</ref> yet imaging survey have identified a possibly two companion red dwarf stars at projected separations 1210 and 1370 [[astronomical unit|AU]], respectively.<ref>{{citation|arxiv=1506.05456|title=A Lucky Imaging search for stellar sources near 74 transit hosts|year=2015|doi=10.1051/0004-6361/201526525|last1=Wöllert|first1=Maria|last2=Brandner|first2=Wolfgang|journal=Astronomy & Astrophysics|volume=579|pages=A129|bibcode=2015A&A...579A.129W|s2cid=118903879}}</ref>
The spectroscopic survey in 2015 have failed to find any stellar companions to it,<ref>{{citation|arxiv=1510.08062|title=Friends of Hot Jupiters III: An Infrared Spectroscopic Search for Low-Mass Stellar Companions|year=2015|doi=10.1088/0004-637X/814/2/148|last1=Piskorz|first1=Danielle|last2=Knutson|first2=Heather A.|last3=Ngo|first3=Henry|last4=Muirhead|first4=Philip S.|last5=Batygin|first5=Konstantin|last6=Crepp|first6=Justin R.|last7=Hinkley|first7=Sasha|last8=Morton|first8=Timothy D.|journal=The Astrophysical Journal|volume=814|issue=2|page=148|bibcode=2015ApJ...814..148P|s2cid=11525988}}</ref> yet imaging survey have identified a possibly two companion red dwarf stars at projected separations 1210 and 1370 [[astronomical unit|AU]], respectively.<ref>{{citation|arxiv=1506.05456|title=A Lucky Imaging search for stellar sources near 74 transit hosts|year=2015|doi=10.1051/0004-6361/201526525|last1=Wöllert|first1=Maria|last2=Brandner|first2=Wolfgang|journal=Astronomy & Astrophysics|volume=579|pages=A129|bibcode=2015A&A...579A.129W|s2cid=118903879}}</ref>


The star was named '''Berehynia''' in December 2019 by the Ukrainian amateur astronomers.<ref name=naming>{{cite web |url=https://news.liga.net/society/news/ukraina-vybrala-imena-dlya-zvezdy-i-ekzoplanety |title=Украина выбрала имена для звезды и экзопланеты |website=LIGA.net |date=18 December 2019 |access-date=2019-12-18}}</ref>
The star was named '''Berehynia''' in December 2019 by Ukrainian amateur astronomers.<ref name=naming>{{cite web |url=https://news.liga.net/society/news/ukraina-vybrala-imena-dlya-zvezdy-i-ekzoplanety |title=Украина выбрала имена для звезды и экзопланеты |website=LIGA.net |date=18 December 2019 |access-date=2019-12-18}}</ref>


==Planetary system==
==Planetary system==
In 2010 a [[Transit (astronomy)|transiting]] hot [[superjovian]] planet [[HAT-P-15b|b]] (named '''Tryzub''' in 2019<ref name=naming/>) was detected. It has an equilibrium temperature of 904{{±|20}} [[Kelvin|K]].<ref name=Kovacs2010/> The orbital simulation shown the planets inward of orbit of [[HAT-P-15b|b]] would in-spiral and be destroyed within time-span of less than billion years.<ref>{{citation|arxiv=1401.7217|title=Small Inner Companions of Warm Jupiters: Lifetimes and Legacies|year=2014|doi=10.1088/0004-637X/778/2/182|last1=Van Laerhoven|first1=Christa|last2=Greenberg|first2=Richard|journal=The Astrophysical Journal|volume=778|issue=2|page=182|s2cid=119297266}}</ref> The planetary orbit is well aligned with the equatorial plane of the star, misalignment equal to 13{{±|6}} degrees.<ref>{{citation|arxiv=2205.10549|year=2022|title=The GAPS Programme at TNG XXXVI. Measurement of the Rossiter-McLaughlin effect and revising the physical and orbital parameters of the HAT-P-15, HAT-P-17, HAT-P-21, HAT-P-26, HAT-P-29 eccentric planetary systems}}</ref>
In 2010 a [[Transit (astronomy)|transiting]] hot [[superjovian]] planet b (named '''Tryzub''' in 2019<ref name=naming/>) was detected. It has an equilibrium temperature of 904{{±|20}} [[Kelvin|K]].<ref name=Kovacs2010/> An orbital simulation shows that any planets inward of the orbit of b would spiral inward and be destroyed within a time-span of less than a billion years.<ref>{{citation|arxiv=1401.7217|title=Small Inner Companions of Warm Jupiters: Lifetimes and Legacies|year=2014|doi=10.1088/0004-637X/778/2/182|last1=Van Laerhoven|first1=Christa|last2=Greenberg|first2=Richard|journal=The Astrophysical Journal|volume=778|issue=2|page=182|s2cid=119297266}}</ref> The planetary orbit is well aligned with the equatorial plane of the star, misalignment equal to 13{{±|6}} degrees.<ref>{{citation|arxiv=2205.10549|year=2022|title=The GAPS Programme at TNG|doi=10.1051/0004-6361/202243742 |last1=Mancini |first1=L. |last2=Esposito |first2=M. |last3=Covino |first3=E. |last4=Southworth |first4=J. |last5=Poretti |first5=E. |last6=Andreuzzi |first6=G. |last7=Barbato |first7=D. |last8=Biazzo |first8=K. |last9=Borsato |first9=L. |last10=Bruni |first10=I. |last11=Damasso |first11=M. |last12=Di Fabrizio |first12=L. |last13=Evans |first13=D. F. |last14=Granata |first14=V. |last15=Lanza |first15=A. F. |last16=Naponiello |first16=L. |last17=Nascimbeni |first17=V. |last18=Pinamonti |first18=M. |last19=Sozzetti |first19=A. |last20=Tregloan-Reed |first20=J. |last21=Basilicata |first21=M. |last22=Bignamini |first22=A. |last23=Bonomo |first23=A. S. |last24=Claudi |first24=R. |last25=Cosentino |first25=R. |last26=Desidera |first26=S. |last27=Fiorenzano |first27=A. F. M. |last28=Giacobbe |first28=P. |last29=Harutyunyan |first29=A. |last30=Henning |first30=Th. |journal=Astronomy & Astrophysics |volume=664 |pages=A162 |s2cid=248986121 |display-authors=1 }}</ref>


[[File:Exoplanet Comparison HAT-P-15 b.png|left|thumb|200px|Size comparison of ''HAT-P-15 b'' and Jupiter]]
[[File:Exoplanet Comparison HAT-P-15 b.png|left|thumb|200px|Size comparison of ''HAT-P-15 b'' and Jupiter]]
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| table_ref = <ref name=Kovacs2010>{{citation|arxiv=1005.5300|title=HAT-P-15b: A 10.9-Day Extrasolar Planet Transiting a Solar-Type Star|year=2010|doi=10.1088/0004-637X/724/2/866|last1=Kovács|first1=G.|last2=Bakos|first2=G. Á.|last3=Hartman|first3=J. D.|last4=Torres|first4=G.|last5=Noyes|first5=R. W.|last6=Latham|first6=D. W.|last7=Howard|first7=A. W.|last8=Fischer|first8=D. A.|last9=Johnson|first9=J. A.|last10=Marcy|first10=G. W.|last11=Isaacson|first11=H.|last12=Sasselov|first12=D. D.|last13=Stefanik|first13=R. P.|last14=Esquerdo|first14=G. A.|last15=Fernandez|first15=J. M.|last16=Lázár|first16=B. Béky J.|last17=Papp|first17=I.|last18=Sári|first18=P.|last19=Sári|first19=P.|journal=The Astrophysical Journal|volume=724|issue=2|pages=866–877|bibcode=2010ApJ...724..866K|s2cid=119207125}}</ref>}}
| table_ref = <ref name=Kovacs2010>{{citation|arxiv=1005.5300|title=HAT-P-15b: A 10.9-Day Extrasolar Planet Transiting a Solar-Type Star|year=2010|doi=10.1088/0004-637X/724/2/866|last1=Kovács|first1=G.|last2=Bakos|first2=G. Á.|last3=Hartman|first3=J. D.|last4=Torres|first4=G.|last5=Noyes|first5=R. W.|last6=Latham|first6=D. W.|last7=Howard|first7=A. W.|last8=Fischer|first8=D. A.|last9=Johnson|first9=J. A.|last10=Marcy|first10=G. W.|last11=Isaacson|first11=H.|last12=Sasselov|first12=D. D.|last13=Stefanik|first13=R. P.|last14=Esquerdo|first14=G. A.|last15=Fernandez|first15=J. M.|last16=Lázár|first16=B. Béky J.|last17=Papp|first17=I.|last18=Sári|first18=P.|last19=Sári|first19=P.|journal=The Astrophysical Journal|volume=724|issue=2|pages=866–877|bibcode=2010ApJ...724..866K|s2cid=119207125}}</ref>}}
{{OrbitboxPlanet
{{OrbitboxPlanet
| exoplanet = [[HAT-P-15b|b]]
| exoplanet = b / Tryzub
| mass = 1.946{{±|0.066}}
| mass = 1.946{{±|0.066}}
| radius = 1.072{{±|0.043}}
| radius = 1.072{{±|0.043}}
Line 67: Line 69:
==References==
==References==
{{Reflist|refs=
{{Reflist|refs=

<ref name="Gaia DR3">{{Cite Gaia DR3|179498266829041664}}</ref>

<ref name=simbad>[http://simbad.u-strasbg.fr/simbad/sim-id?Ident=HAT-P-15 HAT-P-15 -- Star]</ref>
<ref name=simbad>[http://simbad.u-strasbg.fr/simbad/sim-id?Ident=HAT-P-15 HAT-P-15 -- Star]</ref>

}}
}}


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[[Category:Planetary transit variables]]
[[Category:Planetary transit variables]]
[[Category:2MASS objects|J04245952+3927382]]
[[Category:2MASS objects|J04245952+3927382]]
[[Category:Stars with proper names|Berehynia]]


{{main-star-stub}}
{{main-star-stub}}

Latest revision as of 22:27, 24 April 2024

HAT-P-15 / Berehynia
Observation data
Epoch J2000      Equinox J2000
Constellation Perseus
Right ascension 04h 24m 59.5350s[1]
Declination +39° 27′ 38.313″[1]
Apparent magnitude (V) 12.41
Characteristics
Spectral type G5V
Variable type planetary transit[2]
Astrometry
Radial velocity (Rv)31.21 km/s
Proper motion (μ) RA: 14.233(21) mas/yr[1]
Dec.: −9.407(15) mas/yr[1]
Parallax (π)5.1856 ± 0.0166 mas[1]
Distance629 ± 2 ly
(192.8 ± 0.6 pc)
Details[3]
Mass1.013±0.043 M☉
Radius1.080±0.039 R☉
Luminosity1.00±0.11 L☉
Surface gravity (log g)4.38±0.03 cgs
Temperature5684±25 K
Metallicity0.272±0.031
Rotational velocity (v sin i)2.0±0.5 km/s
Age6.8+2.5
−1.6 Gyr
Other designations
Berehynia, Gaia DR3 179498266829041664, TYC 2883-1687-1, GSC 02883-01687, 2MASS J04245952+3927382[4]
Database references
SIMBADdata

HAT-P-15 is a G-type main-sequence star about 630 light-years away. The star is older than Sun yet has a concentration of heavy elements roughly 190% of solar abundance.[3] The star has no noticeable starspot activity.[5]

The spectroscopic survey in 2015 have failed to find any stellar companions to it,[6] yet imaging survey have identified a possibly two companion red dwarf stars at projected separations 1210 and 1370 AU, respectively.[7]

The star was named Berehynia in December 2019 by Ukrainian amateur astronomers.[8]

Planetary system

[edit]

In 2010 a transiting hot superjovian planet b (named Tryzub in 2019[8]) was detected. It has an equilibrium temperature of 904±20 K.[2] An orbital simulation shows that any planets inward of the orbit of b would spiral inward and be destroyed within a time-span of less than a billion years.[9] The planetary orbit is well aligned with the equatorial plane of the star, misalignment equal to 13±6 degrees.[10]

Size comparison of HAT-P-15 b and Jupiter
The HAT-P-15 planetary system[2]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b / Tryzub 1.946±0.066 MJ 0.0964±0.0014 10.863502±0.000027 0.19±0.019 89.1±0.2° 1.072±0.043 RJ

References

[edit]
  1. ^ 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.
  2. ^ a b c Kovács, G.; Bakos, G. Á.; Hartman, J. D.; Torres, G.; Noyes, R. W.; Latham, D. W.; Howard, A. W.; Fischer, D. A.; Johnson, J. A.; Marcy, G. W.; Isaacson, H.; Sasselov, D. D.; Stefanik, R. P.; Esquerdo, G. A.; Fernandez, J. M.; Lázár, B. Béky J.; Papp, I.; Sári, P.; Sári, P. (2010), "HAT-P-15b: A 10.9-Day Extrasolar Planet Transiting a Solar-Type Star", The Astrophysical Journal, 724 (2): 866–877, arXiv:1005.5300, Bibcode:2010ApJ...724..866K, doi:10.1088/0004-637X/724/2/866, S2CID 119207125
  3. ^ a b Teske, Johanna K.; Thorngren, Daniel; Fortney, Jonathan J.; Hinkel, Natalie; Brewer, John M. (2019), "Do Metal-Rich Stars Make Metal-Rich Planets? New Insights on Giant Planet Formation from Host Star Abundances", The Astronomical Journal, 158 (6): 239, arXiv:1912.00255, Bibcode:2019AJ....158..239T, doi:10.3847/1538-3881/ab4f79, S2CID 208527082
  4. ^ HAT-P-15 -- Star
  5. ^ Shkolnik, Evgenya L. (2013), "An Ultraviolet Investigation of Activity on Exoplanet Host Stars", The Astrophysical Journal, 766 (1): 9, arXiv:1301.6192, Bibcode:2013ApJ...766....9S, doi:10.1088/0004-637X/766/1/9, S2CID 118415788
  6. ^ 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
  7. ^ 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
  8. ^ a b "Украина выбрала имена для звезды и экзопланеты". LIGA.net. 18 December 2019. Retrieved 2019-12-18.
  9. ^ Van Laerhoven, Christa; Greenberg, Richard (2014), "Small Inner Companions of Warm Jupiters: Lifetimes and Legacies", The Astrophysical Journal, 778 (2): 182, arXiv:1401.7217, doi:10.1088/0004-637X/778/2/182, S2CID 119297266
  10. ^ Mancini, L.; et al. (2022), "The GAPS Programme at TNG", Astronomy & Astrophysics, 664: A162, arXiv:2205.10549, doi:10.1051/0004-6361/202243742, S2CID 248986121


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