E-viri
Recenzirano
Odprti dostop
-
Huang, Chelsea X.; Quinn, Samuel N.; Vanderburg, Andrew; Becker, Juliette; Rodriguez, Joseph E.; Pozuelos, Francisco J.; Gandolfi, Davide; Zhou, George; Mann, Andrew W.; Collins, Karen A.; Crossfield, Ian; Barkaoui, Khalid; Collins, Kevin I.; Fridlund, Malcolm; Gillon, Michaël; Gonzales, Erica J.; Günther, Maximilian N.; Henry, Todd J.; Howell, Steve B.; James, Hodari-Sadiki; Jao, Wei-Chun; Jehin, Emmanuël; Jensen, Eric L. N.; Kane, Stephen R.; Lissauer, Jack J.; Matthews, Elisabeth; Matson, Rachel A.; Paredes, Leonardo A.; Schlieder, Joshua E.; Stassun, Keivan G.; Shporer, Avi; Sha, Lizhou; Tan, Thiam-Guan; Georgieva, Iskra; Mathur, Savita; Palle, Enric; Persson, Carina M.; Eylen, Vincent Van; Ricker, George R.; Vanderspek, Roland K.; Latham, David W.; Winn, Joshua N.; Seager, S.; Jenkins, Jon M.; Burke, Christopher J.; Goeke, Robert F.; Rinehart, Stephen; Rose, Mark E.; Ting, Eric B.; Torres, Guillermo; Wong, Ian
Astrophysical journal. Letters, 03/2020, Letnik: 892, Številka: 1Journal Article, Web Resource
Hot Jupiters are rarely accompanied by other planets within a factor of a few in orbital distance. Previously, only two such systems have been found. Here, we report the discovery of a third system using data from the Transiting Exoplanet Survey Satellite (TESS). The host star, TOI-1130, is an eleventh magnitude K-dwarf in Gaia G-band. It has two transiting planets: a Neptune-sized planet (3.65 0.10 ) with a 4.1 days period, and a hot Jupiter ( ) with an 8.4 days period. Precise radial-velocity observations show that the mass of the hot Jupiter is . For the inner Neptune, the data provide only an upper limit on the mass of 0.17 (3 ). Nevertheless, we are confident that the inner planet is real, based on follow-up ground-based photometry and adaptive-optics imaging that rule out other plausible sources of the TESS transit signal. The unusual planetary architecture of and the brightness of the host star make TOI-1130 a good test case for planet formation theories, and an attractive target for future spectroscopic observations.
Avtor
![loading ... loading ...](themes/default/img/ajax-loading.gif)
Vnos na polico
Trajna povezava
- URL:
Faktor vpliva
Dostop do baze podatkov JCR je dovoljen samo uporabnikom iz Slovenije. Vaš trenutni IP-naslov ni na seznamu dovoljenih za dostop, zato je potrebna avtentikacija z ustreznim računom AAI.
Leto | Faktor vpliva | Izdaja | Kategorija | Razvrstitev | ||||
---|---|---|---|---|---|---|---|---|
JCR | SNIP | JCR | SNIP | JCR | SNIP | JCR | SNIP |
Baze podatkov, v katerih je revija indeksirana
Ime baze podatkov | Področje | Leto |
---|
Povezave do osebnih bibliografij avtorjev | Povezave do podatkov o raziskovalcih v sistemu SICRIS |
---|
Vir: Osebne bibliografije
in: SICRIS
To gradivo vam je dostopno v celotnem besedilu. Če kljub temu želite naročiti gradivo, kliknite gumb Nadaljuj.