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| ==Planetary system== | ==Planetary system== | ||
| {{OrbitboxPlanet begin | {{OrbitboxPlanet begin | ||
| | table_ref = <ref name="Bonomo2023 |
| table_ref = <ref name="Bonomo2023"/> | ||
| }} | }} | ||
| {{OrbitboxPlanet | {{OrbitboxPlanet | ||
| Line 80: | Line 80: | ||
| }} | }} | ||
| {{OrbitboxPlanet hypothetical | {{OrbitboxPlanet hypothetical | ||
| | exoplanet = e | | exoplanet = e<ref name="Weiss2024"/> | ||
| | mass_earth = {{val|8.1|1.7|p=≥}} | | mass_earth = {{val|8.1|1.7|p=≥}} | ||
| | semimajor = 0.25 | | semimajor = 0.25 | ||
| | period = {{val|50.25|0.15} | | period = {{val|50.25|0.15}} | ||
| | radius_earth = | | radius_earth = | ||
| | inclination = | | inclination = | ||
| Line 105: | Line 105: | ||
| The asteroseismology work was, in part, paid for by the ] program operated by White Dwarf Research Corporation, a ] non-profit organization.<ref name=Slate>{{cite news|title=Astronomers Find the Tiniest Exoplanet Yet|author=Phil Plait|work=Bad Astronomy blog |publisher=Slate|date=February 20, 2013|url=http://www.slate.com/blogs/bad_astronomy/2013/02/20/smallest_exoplanet_kepler_37b_is_barely_bigger_than_earth_s_moon.html|access-date=February 21, 2013}}</ref> | The asteroseismology work was, in part, paid for by the ] program operated by White Dwarf Research Corporation, a ] non-profit organization.<ref name=Slate>{{cite news|title=Astronomers Find the Tiniest Exoplanet Yet|author=Phil Plait|work=Bad Astronomy blog |publisher=Slate|date=February 20, 2013|url=http://www.slate.com/blogs/bad_astronomy/2013/02/20/smallest_exoplanet_kepler_37b_is_barely_bigger_than_earth_s_moon.html|access-date=February 21, 2013}}</ref> | ||
| In 2014, a fourth planet with an orbital period of 51 days (Kepler-37e) was reported based on ]s.<ref name="HaddenLithwick2014"/> Previously this signal was thought to be a false positive due to its low signal-to-noise ratio, and indeed later studies failed to detect either the transit or TTV signal. A study in 2021 again found that the TTV data disfavors the presence of planet e, and argued that it should be stripped of its "confirmed planet" status.<ref name=Rajpaul2021/>{{rp| |
In 2014, a fourth planet with an orbital period of 51 days (Kepler-37e) was reported based on ]s.<ref name="HaddenLithwick2014"/> Previously this signal was thought to be a false positive due to its low signal-to-noise ratio, and indeed later studies failed to detect either the transit or TTV signal. A study in 2021 again found that the TTV data disfavors the presence of planet e, and argued that it should be stripped of its "confirmed planet" status.<ref name=Rajpaul2021/>{{rp|3–4,18–19}} | ||
| A 2023 study modeled the system both with and without a planet candidate at 51 days. Based on the assumption that a planet with a circular orbit of about 51 days is present, marginal ] evidence was found for a sub-Neptune mass planet. Evidence of a longer-period planet candidate was also found. No additional planet has been confirmed, and the system remains with three confirmed planets.<ref name="Weiss2024"/>{{rp| |
A 2023 study modeled the system both with and without a planet candidate at 51 days. Based on the assumption that a planet with a circular orbit of about 51 days is present, marginal ] evidence was found for a sub-Neptune mass planet. Evidence of a longer-period planet candidate was also found. No additional planet has been confirmed, and the system remains with three confirmed planets.<ref name="Weiss2024"/>{{rp|37–38}} | ||
| ==Notes== | ==Notes== | ||
| Line 123: | Line 123: | ||
| <ref name="HaddenLithwick2014">{{cite journal | bibcode = 2014ApJ...787...80H | title=Densities and Eccentricities of 139 Kepler Planets from Transit Time Variations | journal=The Astrophysical Journal | volume=787 | issue=1 | pages=80 | year=2014 |author=Hadden, Sam |author2=Lithwick, Yoram| doi=10.1088/0004-637X/787/1/80 |arxiv = 1310.7942 | s2cid=119097836 }}</ref> | <ref name="HaddenLithwick2014">{{cite journal | bibcode = 2014ApJ...787...80H | title=Densities and Eccentricities of 139 Kepler Planets from Transit Time Variations | journal=The Astrophysical Journal | volume=787 | issue=1 | pages=80 | year=2014 |author=Hadden, Sam |author2=Lithwick, Yoram| doi=10.1088/0004-637X/787/1/80 |arxiv = 1310.7942 | s2cid=119097836 }}</ref> | ||
| <ref name=Rajpaul2021>{{citation|arxiv=2107.13900|year=2021|title=A HARPS-N mass for the elusive Kepler-37d: A case study in disentangling stellar activity and planetary signals|doi=10.1093/mnras/stab2192|last1=Rajpaul|first1=V. M.|last2=Buchhave|first2=L. A.|last3=Lacedelli|first3=G.|last4=Rice|first4=K.|last5=Mortier|first5=A.|last6=Malavolta|first6=L.|last7=Aigrain|first7=S.|last8=Borsato|first8=L.|last9=Mayo|first9=A. W.|last10=Charbonneau|first10=D.|last11=Damasso|first11=M.|last12=Dumusque|first12=X.|last13=Ghedina|first13=A.|last14=Latham|first14=D. W.|last15=López-Morales|first15=M.|last16=Magazzù|first16=A.|last17=Micela|first17=G.|last18=Molinari|first18=E.|last19=Pepe|first19=F.|last20=Piotto|first20=G.|last21=Poretti|first21=E.|last22=Rowther|first22=S.|last23=Sozzetti|first23=A.|last24=Udry|first24=S.|last25=Watson|first25=C. A.|journal=Monthly Notices of the Royal Astronomical Society|volume=507|issue=2|pages=1847–1868 |bibcode=2021MNRAS.507.1847R}}</ref> | <ref name=Rajpaul2021>{{citation|arxiv=2107.13900|year=2021|title=A HARPS-N mass for the elusive Kepler-37d: A case study in disentangling stellar activity and planetary signals|doi=10.1093/mnras/stab2192|last1=Rajpaul|first1=V. M.|last2=Buchhave|first2=L. A.|last3=Lacedelli|first3=G.|last4=Rice|first4=K.|last5=Mortier|first5=A.|last6=Malavolta|first6=L.|last7=Aigrain|first7=S.|last8=Borsato|first8=L.|last9=Mayo|first9=A. W.|last10=Charbonneau|first10=D.|last11=Damasso|first11=M.|last12=Dumusque|first12=X.|last13=Ghedina|first13=A.|last14=Latham|first14=D. W.|last15=López-Morales|first15=M.|last16=Magazzù|first16=A.|last17=Micela|first17=G.|last18=Molinari|first18=E.|last19=Pepe|first19=F.|last20=Piotto|first20=G.|last21=Poretti|first21=E.|last22=Rowther|first22=S.|last23=Sozzetti|first23=A.|last24=Udry|first24=S.|last25=Watson|first25=C. A.|journal=Monthly Notices of the Royal Astronomical Society|volume=507|issue=2|pages=1847–1868 |doi-access=free |bibcode=2021MNRAS.507.1847R}}</ref> | ||
| <ref name="Bonomo2023">{{cite journal |last1=Bonomo |first1=A. S. |last2=Dumusque |first2=X. |display-authors=etal |date=September 2023 |title=Cold Jupiters and improved masses in 38 Kepler and K2 small planet systems from 3661 HARPS-N radial velocities. No excess of cold Jupiters in small planet systems |journal=] |volume=677 |issue= |pages=A33 |doi=10.1051/0004-6361/202346211 |arxiv=2304.05773 |bibcode=2023A&A...677A..33B |s2cid=258078829}}</ref> | <ref name="Bonomo2023">{{cite journal |last1=Bonomo |first1=A. S. |last2=Dumusque |first2=X. |display-authors=etal |date=September 2023 |title=Cold Jupiters and improved masses in 38 Kepler and K2 small planet systems from 3661 HARPS-N radial velocities. No excess of cold Jupiters in small planet systems |journal=] |volume=677 |issue= |pages=A33 |doi=10.1051/0004-6361/202346211 |arxiv=2304.05773 |bibcode=2023A&A...677A..33B |s2cid=258078829}}</ref> | ||
| <ref name="Weiss2024">{{cite journal | title=The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory | |
<ref name="Weiss2024">{{cite journal | title=The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory | last1=Weiss | first1=Lauren M. | last2=Isaacson | first2=Howard | last3=Howard | first3=Andrew W. | last4=Fulton | first4=Benjamin J. | last5=Petigura | first5=Erik A. | last6=Fabrycky | first6=Daniel | last7=Jontof-Hutter | first7=Daniel | last8=Steffen | first8=Jason H. | last9=Schlichting | first9=Hilke E. | last10=Wright | first10=Jason T. | last11=Beard | first11=Corey | last12=Brinkman | first12=Casey L. | last13=Chontos | first13=Ashley | last14=Giacalone | first14=Steven | last15=Hill | first15=Michelle L. | last16=Kosiarek | first16=Molly R. | last17=MacDougall | first17=Mason G. | last18=Močnik | first18=Teo | last19=Polanski | first19=Alex S. | last20=Turtelboom | first20=Emma V. | last21=Tyler | first21=Dakotah | last22=Van Zandt | first22=Judah | display-authors=1 | journal=The Astrophysical Journal Supplement Series | volume=270 | issue=1 | date=2024-01-01 | article-number=8 | page=<!-- to prevent citation bot adding nonexistent page number--> | arxiv=2304.00071 | bibcode=2024ApJS..270....8W | bibcode-access=free | doi=10.3847/1538-4365/ad0cab | doi-access=free }}</ref> | ||
| }} | }} | ||
| Line 140: | Line 140: | ||
| {{Kepler-37}} | {{Kepler-37}} | ||
| {{Stars of Lyra}} | {{Stars of Lyra}} | ||
| ] | ] | ||
Latest revision as of 05:26, 23 August 2024
G-type main-sequence star in the constellation Lyra Line up comparing the planets in the Kepler-37 system to the Moon and planets in the Solar System. | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Lyra |
| Right ascension | 18 56 14.30760 |
| Declination | +44° 31′ 05.3896″ |
| Apparent magnitude (V) | 9.710 |
| Characteristics | |
| Spectral type | G8V |
| Astrometry | |
| Radial velocity (Rv) | −30.92±0.20 km/s |
| Proper motion (μ) | RA: −60.396 mas/yr Dec.: 48.657 mas/yr |
| Parallax (π) | 15.6253 ± 0.0105 mas |
| Distance | 208.7 ± 0.1 ly (64.00 ± 0.04 pc) |
| Details | |
| Mass | 0.79+0.033 −0.03 M☉ |
| Radius | 0.789+0.0064 −0.0056 R☉ |
| Temperature | 5357±68 K |
| Metallicity | −0.36±0.05 dex |
| Rotational velocity (v sin i) | 1.1 (± 1.1) km/s |
| Age | 7.6+3.4 −3.1 Gyr |
| Other designations | |
| KOI-245, KIC 8478994, TYC 3131-1199-1, BD+44 3020, 2MASS J18561431+4431052, GSC 03131-01199, Gaia DR2 2106674071344722688 | |
| Database references | |
| SIMBAD | data |
| KIC | data |
Kepler-37, also known as UGA-1785, is a G-type main-sequence star located in the constellation Lyra 209 light-years (64 parsecs) from Earth. It is host to exoplanets Kepler-37b, Kepler-37c, Kepler-37d and possibly Kepler-37e, all of which orbit very close to it. Kepler-37 has a mass about 80.3 percent of the Sun's and a radius about 77 percent as large. It has a temperature similar to that of the Sun, but a bit cooler at 5,357 K. It has about half the metallicity of the Sun. With an age of roughly 6 billion years, it is slightly older than the Sun, but is still a main-sequence star. Until January 2015, Kepler-37 was the smallest star to be measured via asteroseismology.
Planetary system
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | <0.79 M🜨 | 0.1019±0.0014 | 13.367020(60) | <0.098 | 88.63+0.30 −0.53° |
0.3098+0.0059 −0.0076 R🜨 |
| c | <1.3 M🜨 | 0.1390±0.0020 | 21.301848(18) | <0.099 | 89.07+0.19 −0.33° |
0.755+0.033 −0.055 R🜨 |
| d | <2.0 M🜨 | 0.2109±0.0030 | 39.7922622(65) | <0.10 | 89.335+0.043 −0.047° |
2.030+0.030 −0.039 R🜨 |
| e (disputed) | ≥8.1±1.7 M🜨 | 0.25 | 50.25±0.15 | — | — | — |
Kepler-37b is the closest planet to Kepler-37. At the time of its discovery in February 2013, it was the smallest known exoplanet. At 3,865 kilometres (2,402 mi) in diameter, it is slightly larger than the Moon. It orbits Kepler-37 once every 13 days at a distance of about 0.1 astronomical units (AU). Kepler-37b has a rocky surface and is believed to be too small and too close to its star to support water or maintain an atmosphere. Surface temperature is estimated at 700 K (427 °C; 800 °F).
Kepler-37c is around three-quarters of the diameter of Earth and orbits approximately every 21 days at a distance of just under 0.14 AU. Kepler-37d is about twice the diameter of Earth. It orbits in around 40 days at a distance of nearly 0.21 AU. Neither are able to support liquid water due to their proximity to Kepler-37.
A 2021 study detected Kepler-37d via radial velocity, finding a mass of about 5.4 ME, but a 2023 study instead found an upper limit on its mass of only 2 ME. In either case, it is not a rocky planet, but a low-density planet rich in volatiles. The periods of the three inner planets are close (within one per cent) to a 5:8:15 mean-motion resonance relationship.
In 2015, a grant was approved to further expand the Sagan Planet Walk by installing a Kepler-37d station on the Moon 384,500 kilometers (238,900 mi) away.
Discovery
The Kepler-37 planets were discovered in September 2012 with the aid of transit events detected by the Kepler space telescope, and announced to the public in February 2013. Computer simulation was used to rule out other astronomical phenomena mimicking planetary transits with probabilities of error <0.05% (3σ) for each potential planet. Additionally, simulation demonstrated that the proposed planetary configuration was stable. The exoplanets were considerably smaller than any previously detected, leading Science World Reports to state that "a major technological improvement for the telescope" had been achieved.
Thomas Barclay, an astrophysicist on the Kepler space telescope team, said the discovery was "really good news" in the search for hospitable planets, a prime objective of the project, because it demonstrated the telescope was capable of detecting Earth-sized planets. However, he does not anticipate finding many planets as small as Kepler-37b due to the very small amount of light such planets obscure. According to NASA scientist Jack Lissauer, the discovery of Kepler-37b "suggests such little planets are common, and more planetary wonders await as we continue to gather and analyze additional data." Astronomer John Johnson of Caltech university said the discovery would have been "unimaginable" a few years ago and that the telescope had revolutionized astronomers' picture of the universe.
The asteroseismology work was, in part, paid for by the Nonprofit Adopt a Star program operated by White Dwarf Research Corporation, a crowd funded non-profit organization.
In 2014, a fourth planet with an orbital period of 51 days (Kepler-37e) was reported based on transit-timing variations. Previously this signal was thought to be a false positive due to its low signal-to-noise ratio, and indeed later studies failed to detect either the transit or TTV signal. A study in 2021 again found that the TTV data disfavors the presence of planet e, and argued that it should be stripped of its "confirmed planet" status.
A 2023 study modeled the system both with and without a planet candidate at 51 days. Based on the assumption that a planet with a circular orbit of about 51 days is present, marginal radial velocity evidence was found for a sub-Neptune mass planet. Evidence of a longer-period planet candidate was also found. No additional planet has been confirmed, and the system remains with three confirmed planets.
Notes
- Masses more than a few times that of the Moon result in unphysically high densities.
References
- ^ 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.
- ^ "Kepler Host Star Characteristics". Archive for Space Telescopes. STSI. 2012-02-24. Retrieved 2013-02-21.
- ^ Bonomo, A. S.; Dumusque, X.; et al. (September 2023). "Cold Jupiters and improved masses in 38 Kepler and K2 small planet systems from 3661 HARPS-N radial velocities. No excess of cold Jupiters in small planet systems". Astronomy & Astrophysics. 677: A33. arXiv:2304.05773. Bibcode:2023A&A...677A..33B. doi:10.1051/0004-6361/202346211. S2CID 258078829.
- ^ Barclay, T.; Rowe, J. F.; Lissauer, J. J.; Huber, D.; Fressin, F.; Howell, S. B.; Bryson, S. T.; Chaplin, W. J.; Désert, J.-M.; Lopez, Eric D.; Marcy, Geoffrey W.; Mullally, Fergal; Ragozzine, Darin; Torres, Guillermo; Adams, Elisabeth R.; Agol, Eric; Barrado, David; Basu, Sarbani; Bedding, Timothy R.; Buchhave, Lars A.; Charbonneau, David; Christiansen, Jessie L.; Christensen-Dalsgaard, Jørgen; Ciardi, David; Cochran, William D.; Dupree, Andrea K.; Elsworth, Yvonne; Everett, Mark; Fischer, Debra A.; et al. (2013-02-20). "A sub-Mercury-sized exoplanet". Nature. 494 (7438): 452–4. arXiv:1305.5587. Bibcode:2013Natur.494..452B. doi:10.1038/nature11914. ISSN 0028-0836. PMID 23426260. S2CID 205232792.
- "TYC 3131-1199-1". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2013-02-22.
- Planets in Kepler-37 star system designated ‘UGA-1785’ by NASA
- 211 light years away, star system named for UGA
- Kepler-37, Open Exoplanet catalogue
- Smallest Alien Planet Kepler-37b Explained (Infographic)
- ^ "NASA's Kepler Mission Discovers Tiny Planet System" (Press release). NASA. February 20, 2012. Retrieved February 21, 2012.
- ^ Weiss, Lauren M.; et al. (2024-01-01). "The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory". The Astrophysical Journal Supplement Series. 270 (1) 8. arXiv:2304.00071. Bibcode:2024ApJS..270....8W. doi:10.3847/1538-4365/ad0cab.
- ^ Catherine Griffin (February 21, 2013). "Tiniest Planet Yet Discovered by NASA Outside our Solar System". Science World Report. Retrieved February 21, 2013.
- ^ Rajpaul, V. M.; Buchhave, L. A.; Lacedelli, G.; Rice, K.; Mortier, A.; Malavolta, L.; Aigrain, S.; Borsato, L.; Mayo, A. W.; Charbonneau, D.; Damasso, M.; Dumusque, X.; Ghedina, A.; Latham, D. W.; López-Morales, M.; Magazzù, A.; Micela, G.; Molinari, E.; Pepe, F.; Piotto, G.; Poretti, E.; Rowther, S.; Sozzetti, A.; Udry, S.; Watson, C. A. (2021), "A HARPS-N mass for the elusive Kepler-37d: A case study in disentangling stellar activity and planetary signals", Monthly Notices of the Royal Astronomical Society, 507 (2): 1847–1868, arXiv:2107.13900, Bibcode:2021MNRAS.507.1847R, doi:10.1093/mnras/stab2192
- "Tompkins County Strategic Tourism Planning Board" (PDF). Tompkins County NY. April 15, 2015. Archived from the original (PDF) on December 27, 2016. Retrieved March 5, 2016.
- ^ Eryn Brown (February 21, 2013). "NASA, using Kepler space telescope, finds smallest planet yet". LA Times. Retrieved February 21, 2013.
- Phil Plait (February 20, 2013). "Astronomers Find the Tiniest Exoplanet Yet". Bad Astronomy blog. Slate. Retrieved February 21, 2013.
- Hadden, Sam; Lithwick, Yoram (2014). "Densities and Eccentricities of 139 Kepler Planets from Transit Time Variations". The Astrophysical Journal. 787 (1): 80. arXiv:1310.7942. Bibcode:2014ApJ...787...80H. doi:10.1088/0004-637X/787/1/80. S2CID 119097836.
Further reading
- Barclay, Thomas; et al. (2013). "A sub-Mercury-sized exoplanet". Nature. 494 (7438): 452–4. arXiv:1305.5587. Bibcode:2013Natur.494..452B. doi:10.1038/nature11914. ISSN 0028-0836. PMID 23426260. S2CID 205232792. (Supplementary information)
External links
Media related to Kepler-37 at Wikimedia Commons- Table of confirmed planets at NASA, Kepler mission
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| Constellation of Lyra | |||||||||||||||
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