Astronomy:HIP 67522 b: Difference between revisions
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{{Infobox planet | {{Infobox planet | ||
| extrasolarplanet = yes | | extrasolarplanet = yes | ||
| Line 14: | Line 12: | ||
| discovered = 2020 | | discovered = 2020 | ||
| discovery_method = [[Astronomy:Transit|Primary Transit]] | | discovery_method = [[Astronomy:Transit|Primary Transit]] | ||
| alt_names = HD 120411 b, [[Engineering:Gaia (spacecraft)|Gaia DR2]] 6113920619134019456 b, TYC 7794-2268-1 b<ref>{{cite web|url=http://www.openexoplanetcatalogue.com/planet/HIP%2067522%20b/|title=HIP 67522|publisher=Open Exoplanet Catalogue|accessdate=January 25, 2022}}</ref> | | alt_names = [[Astronomy:Henry Draper Catalogue|HD]] 120411 b, [[Engineering:Gaia (spacecraft)|Gaia DR2]] 6113920619134019456 b, TYC 7794-2268-1 b<ref>{{cite web|url=http://www.openexoplanetcatalogue.com/planet/HIP%2067522%20b/|title=HIP 67522|publisher=Open Exoplanet Catalogue|accessdate=January 25, 2022}}</ref> | ||
| orbit_ref = | | orbit_ref = | ||
| periastron = | | periastron = | ||
| Line 20: | Line 18: | ||
| semimajor = | | semimajor = | ||
| avg_speed = | | avg_speed = | ||
| eccentricity = {{val|0.059|0.193|0.046}}<ref name="HIP">{{cite | | eccentricity = {{val|0.059|0.193|0.046}}<ref name="HIP">{{cite encyclopedia|url=https://exoplanet.eu/catalog/hip_67522_b--7401/|title=Planet HIP 67522 b|date=1995 |encyclopedia=[[Astronomy:Extrasolar Planets Encyclopaedia|Extrasolar Planets Encyclopaedia]]|access-date=January 23, 2022}}</ref> | ||
| period = {{val|6.959503|0.000016}} [[Day|d]]<ref name="HIP"/> | | period = {{val|6.959503|0.000016}} [[Day|d]]<ref name="HIP"/> | ||
| synodic_period = | | synodic_period = | ||
| inclination = {{val|89.34|0.45|0.54|u=deg}} (to plane of sky)<ref name="17M"/><br/>{{val|5.8|2.8|5.7}} [[Degree (angle)|°]] (to host star's equator, projected)<ref name="17Mb"/> | | inclination = {{val|89.34|0.45|0.54|u=deg}} (to plane of sky)<ref name="17M"/><br/>{{val|5.8|2.8|5.7}} [[Degree (angle)|°]] (to host star's equator, projected)<ref name="17Mb">{{cite journal|last1=Heitzmann|first1=A.|last2=Zhou|first2=G.|last3=Quinn|first3=S. N.|last4=Marsden|first4=S. C.|last5=Wright|first5=D.|last6=Petit|first6=P.|last7=Vanderburg|first7=A. M.|last8=Bouma|first8=L. G.|last9=Mann|first9=A. W.|last10=Rizzuto|first10=A. C.|date=November 12, 2021|title=The Obliquity of HIP 67522 b: A 17 Myr Old Transiting Hot, Jupiter-sized Planet|journal=The Astrophysical Journal Letters|volume=922|issue=1|page=L1|arxiv=2109.04174|doi=10.3847/2041-8213/ac3485|bibcode=2021ApJ...922L...1H|s2cid=237452642 |doi-access=free }}</ref> | ||
| angular_dist = | | angular_dist = | ||
| long_periastron = | | long_periastron = | ||
| Line 31: | Line 29: | ||
| star = HIP 67522 | | star = HIP 67522 | ||
| physical_ref = | | physical_ref = | ||
| mean_radius = {{val|0. | | mean_radius = {{val|0.897|0.051}} {{Jupiter radius|link=y}}<ref name="HIP"/> | ||
| volume = | | volume = | ||
| density = {{val|0. | | density = {{val|0.10|p=<|ul=g/cm3}}<ref name="ab"/><ref name=thao/> | ||
| mass = < | | mass = 13.8 ± 1.0, <20 {{Earth mass|sym=y|link=y}}<ref name="ab"/><ref name=thao/> | ||
| surface_grav = | | surface_grav = | ||
| moment_of_inertia_factor = | | moment_of_inertia_factor = | ||
| Line 42: | Line 40: | ||
}} | }} | ||
'''HIP 67522 b''' is a [[Astronomy:Hot | '''HIP 67522 b''' is a [[Astronomy:Hot Neptune|hot Neptune]] or sub-Saturn exoplanet orbiting the [[Astronomy:G-type main-sequence star|G-type star]]<ref name="NASA">{{cite web|url=https://exoplanets.nasa.gov/exoplanet-catalog/7659/hip-67522-b/|title=HIP 67522 b|date=24 July 2020 |publisher=exoplanets.nasa.gov|accessdate=January 23, 2022}}</ref> HIP 67522, approximately 415 light-years from [[HandWiki:Earth|Earth]]<ref name="NASA"/> in the constellation [[Astronomy:Centaurus|Centaurus]].<ref name=thao>{{Cite journal |last1=Thao |first1=Pa Chia |last2=Mann |first2=Andrew W. |last3=Feinstein |first3=Adina D. |last4=Gao |first4=Peter |last5=Thorngren |first5=Daniel |last6=Rotman |first6=Yoav |last7=Welbanks |first7=Luis |last8=Brown |first8=Alexander |last9=Duvvuri |first9=Girish M. |last10=France |first10=Kevin |last11=Longo |first11=Isabella |last12=Sandoval |first12=Angeli |last13=Schneider |first13=P. Christian |last14=Wilson |first14=David J. |last15=Youngblood |first15=Allison |date=2024-12-01 |title=The Featherweight Giant: Unraveling the Atmosphere of a 17 Myr Planet with JWST |journal=The Astronomical Journal |volume=168 |issue=6 |pages=297 |arxiv=2409.16355 |bibcode=2024AJ....168..297T |doi=10.3847/1538-3881/ad81d7 |doi-access=free |issn=0004-6256}}</ref> It was discovered using the [[Astronomy:Transiting Exoplanet Survey Satellite|Transiting Exoplanet Survey Satellite]] (TESS). It is one of the youngest transiting planets of any type, and one of only four others less than 100 million years old (along with [[Astronomy:AU Microscopii b|AU Mic b]], [[Astronomy:V1298 Tauri|V1298 Tau c]], [[Astronomy:DS Tucanae|DS Tuc Ab]] and TOI-942 b) to have the angle between its orbit and its host star's rotation measured, at {{val|5.8|2.8|5.7}} degrees.<ref name="17Mb"/> This planet, in turn, may help in understanding how other hot Neptunes form. | ||
Due to its young age, it has not reached its final size | Due to its young age, it has not reached its final size. Also due to the [[Astronomy:Kelvin–Helmholtz mechanism|Kelvin–Helmholtz mechanism]],<ref name="17Mb"/> which occurs as a result of the planet itself cooling, its internal pressure drops, which will in turn cause the planet to shrink. Its final size will depend on the composition of its [[Astronomy:Planetary core|core]].<ref>{{cite journal|last1=Lopez|first1=E. D.|last2=Fortney|first2=J. J.|title=The Role of Core Mass in Controlling Evaporation: The Kepler Radius Distribution and the Kepler-36 Density Dichotomy|date=September 17, 2013|url=https://iopscience.iop.org/article/10.1088/0004-637X/776/1/2/meta|journal=The Astrophysical Journal|volume=776|issue=1|page=2|arxiv=1305.0269|doi=10.1088/0004-637X/776/1/2|bibcode=2013ApJ...776....2L|s2cid=118545757 }}</ref> | ||
There is also evidence that another planet might also be present in the planetary system.<ref name="17M"/> | There is also evidence that another planet might also be present in the planetary system.<ref name="17M"/> | ||
It was shown in 2024 that HIP 67522 b is one of the [[Astronomy:List of exoplanet extremes|least dense]] known planets, with a density less than 0.10 g/cm<sup>3</sup>. It might have formed beyond the water-[[Physics:Frost line (astrophysics)|snowline]], where the contamination by both rocky and [[Astronomy:Ice giant|icy]] materials frequently takes place.<ref name="ab">{{cite news|last=Cowing|first=Keith|title=The Featherweight Giant: Unraveling the Atmosphere of a 17 Myr Planet with JWST|url=https://astrobiology.com/2024/10/the-featherweight-giant-unraveling-the-atmosphere-of-a-17-myr-planet-with-jwst.html|website=Astrobiology|date=8 October 2024|accessdate=11 October 2024}}</ref><ref name=thao/> In 2025, it was revealed with certainty that HIP 67522 b triggers the increase in flare from the host star via the star-planet [[Physics:Magnetism|magnetic]] interactions. These flares might have caused the shrinkage of the planet's atmosphere.<ref>{{Cite journal |last1=Ilin |first1=Ekaterina |last2=Vedantham |first2=Harish K. |last3=Poppenhäger |first3=Katja |last4=Bloot |first4=Sanne |last5=Callingham |first5=Joseph R. |last6=Brandeker |first6=Alexis |last7=Chakraborty |first7=Hritam |date=2025-07-02 |title=Close-in planet induces flares on its host star |url=https://www.nature.com/articles/s41586-025-09236-z |journal=Nature |language=en |pages=1–4 |doi=10.1038/s41586-025-09236-z |pmid=40604272 |issn=1476-4687 |url-access=subscription }}</ref> | |||
==References== | ==References== | ||
Latest revision as of 21:48, 3 September 2025
| Discovery[1] | |
|---|---|
| Discovered by | THYME (Rizzuto et al.) |
| Discovery date | 2020 |
| Primary Transit | |
| Designations | |
| HD 120411 b, Gaia DR2 6113920619134019456 b, TYC 7794-2268-1 b[2] | |
| Orbital characteristics | |
| Eccentricity | 0.059+0.193 −0.046[3] |
| Orbital period | 6.959503±0.000016 d[3] |
| Inclination | 89.34°+0.45° −0.54° (to plane of sky)[1] 5.8+2.8 −5.7 ° (to host star's equator, projected)[4] |
| 343.0+92.0 −140.0 °[3] | |
| Star | HIP 67522 |
| Physical characteristics | |
| Mean radius | 0.897±0.051 |♃|J}}}}}}[3] |
| Mass | 13.8 ± 1.0, <20 M⊕[5][6] |
| Mean density | <0.10 g/cm3[5][6] |
| Physics | 1174±21 K[3] |
HIP 67522 b is a hot Neptune or sub-Saturn exoplanet orbiting the G-type star[7] HIP 67522, approximately 415 light-years from Earth[7] in the constellation Centaurus.[6] It was discovered using the Transiting Exoplanet Survey Satellite (TESS). It is one of the youngest transiting planets of any type, and one of only four others less than 100 million years old (along with AU Mic b, V1298 Tau c, DS Tuc Ab and TOI-942 b) to have the angle between its orbit and its host star's rotation measured, at 5.8+2.8
−5.7 degrees.[4] This planet, in turn, may help in understanding how other hot Neptunes form.
Due to its young age, it has not reached its final size. Also due to the Kelvin–Helmholtz mechanism,[4] which occurs as a result of the planet itself cooling, its internal pressure drops, which will in turn cause the planet to shrink. Its final size will depend on the composition of its core.[8]
There is also evidence that another planet might also be present in the planetary system.[1]
It was shown in 2024 that HIP 67522 b is one of the least dense known planets, with a density less than 0.10 g/cm3. It might have formed beyond the water-snowline, where the contamination by both rocky and icy materials frequently takes place.[5][6] In 2025, it was revealed with certainty that HIP 67522 b triggers the increase in flare from the host star via the star-planet magnetic interactions. These flares might have caused the shrinkage of the planet's atmosphere.[9]
References
- ↑ 1.0 1.1 1.2 Rizzuto, A. C.; Newton, E. R.; Mann, A. W.; Tofflemire, B. M.; Vanderburg, A.; Kraus, A. L.; Wood, M. L.; Quinn, S. N. et al. (June 22, 2020). "TESS Hunt for Young and Maturing Exoplanets (THYME). II. A 17 Myr Old Transiting Hot Jupiter in the Sco-Cen Association". The Astronomical Journal 160 (1): 33. doi:10.3847/1538-3881/ab94b7. Bibcode: 2020AJ....160...33R.
- ↑ "HIP 67522". Open Exoplanet Catalogue. http://www.openexoplanetcatalogue.com/planet/HIP%2067522%20b/. Retrieved January 25, 2022.
- ↑ 3.0 3.1 3.2 3.3 3.4 "Planet HIP 67522 b". Extrasolar Planets Encyclopaedia. 1995. https://exoplanet.eu/catalog/hip_67522_b--7401/. Retrieved January 23, 2022.
- ↑ 4.0 4.1 4.2 Heitzmann, A.; Zhou, G.; Quinn, S. N.; Marsden, S. C.; Wright, D.; Petit, P.; Vanderburg, A. M.; Bouma, L. G. et al. (November 12, 2021). "The Obliquity of HIP 67522 b: A 17 Myr Old Transiting Hot, Jupiter-sized Planet". The Astrophysical Journal Letters 922 (1): L1. doi:10.3847/2041-8213/ac3485. Bibcode: 2021ApJ...922L...1H.
- ↑ 5.0 5.1 5.2 Cowing, Keith (8 October 2024). "The Featherweight Giant: Unraveling the Atmosphere of a 17 Myr Planet with JWST". https://astrobiology.com/2024/10/the-featherweight-giant-unraveling-the-atmosphere-of-a-17-myr-planet-with-jwst.html. Retrieved 11 October 2024.
- ↑ 6.0 6.1 6.2 6.3 Thao, Pa Chia; Mann, Andrew W.; Feinstein, Adina D.; Gao, Peter; Thorngren, Daniel; Rotman, Yoav; Welbanks, Luis; Brown, Alexander et al. (2024-12-01). "The Featherweight Giant: Unraveling the Atmosphere of a 17 Myr Planet with JWST". The Astronomical Journal 168 (6): 297. doi:10.3847/1538-3881/ad81d7. ISSN 0004-6256. Bibcode: 2024AJ....168..297T.
- ↑ 7.0 7.1 "HIP 67522 b". exoplanets.nasa.gov. 24 July 2020. https://exoplanets.nasa.gov/exoplanet-catalog/7659/hip-67522-b/. Retrieved January 23, 2022.
- ↑ Lopez, E. D.; Fortney, J. J. (September 17, 2013). "The Role of Core Mass in Controlling Evaporation: The Kepler Radius Distribution and the Kepler-36 Density Dichotomy". The Astrophysical Journal 776 (1): 2. doi:10.1088/0004-637X/776/1/2. Bibcode: 2013ApJ...776....2L. https://iopscience.iop.org/article/10.1088/0004-637X/776/1/2/meta.
- ↑ Ilin, Ekaterina; Vedantham, Harish K.; Poppenhäger, Katja; Bloot, Sanne; Callingham, Joseph R.; Brandeker, Alexis; Chakraborty, Hritam (2025-07-02). "Close-in planet induces flares on its host star" (in en). Nature: 1–4. doi:10.1038/s41586-025-09236-z. ISSN 1476-4687. PMID 40604272. https://www.nature.com/articles/s41586-025-09236-z.
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