An extrasolar planet that transits the disk of its parent star

Konacki, Maciej; Torres, Guillermo; Jha, Saurabh W.; Sasselov, Dimitar

doi:10.1038/nature01379

Cited by 303 publications

(301 citation statements)

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“…Many candidates were discovered by the OGLE team who carried out systematic searches, monitoring millions of stars along fields located in the Milky Way disk (Udalski et al 2002a(Udalski et al ,b, 2003Pont et al 2008). Of more than 200 transiting candidates, already seven OGLE transits have been confirmed as being due to planets: OGLE-TR-10 ( Konacki et al 2005), OGLE-TR-56 (Konacki et al 2003), OGLE-TR-111 ), OGLE-TR-113 Konacki et al 2004), OGLE-TR-132 ), OGLE-TR-182 ), OGLE-TR-211 . Most of the other targets are eclipsing low-mass stars or brown dwarfs, or are due to blends of normal stars, triplets, etc.…”

Section: Introductionmentioning

confidence: 99%

Millimagnitude photometry for transiting extrasolar planetary candidates

Pietrukowicz¹,

Minniti²,

Díaz³

et al. 2010

A&A

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Aims. We used VLT/VIMOS images in the V band to obtain light curves of the extrasolar planetary transits OGLE-TR-111 and OGLE-TR-113 and the candidate planetary transits: OGLE-TR-82, OGLE-TR-86, OGLE-TR-91, OGLE-TR-106, OGLE-TR-109, OGLE-TR-110, OGLE-TR-159, OGLE-TR-167, OGLE-TR-170, OGLE-TR-171. Methods. Using difference imaging photometry, we were able to achieve millimagnitude errors in the individual data points. We present the analysis of the data and the light curves by measuring transit amplitudes and ephemerides and by calculating geometrical parameters for some of the systems. Results. We observed nine OGLE objects at the predicted transit moments. Two other transits were shifted in time by a few hours. For another seven objects we expected to observe transits during the VIMOS run, but they were not detected. Conclusions. The stars OGLE-TR-111 and OGLE-TR-113 are probably the only OGLE objects in the observed sample to host planets, with the other objects being very likely eclipsing binaries or multiple systems. In this paper we also report on four new transiting candidates which we have found in the data.

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Section: Introductionmentioning

confidence: 99%

Millimagnitude photometry for transiting extrasolar planetary candidates

Pietrukowicz¹,

Minniti²,

Díaz³

et al. 2010

A&A

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“…The first transiting planet, HD 209458b, was found through photometric follow-up of a RV detection [7][8] . Subsequently, five of the transiting candidates found by the OGLE survey 9 have been confirmed as having planetary masses through RV measurements [10][11][12][13][14] , and four other planets around bright field stars have been found in separate transit surveys [15][16][17][18] . These ten RVconfirmed transiting planets have periods between 1.2 and 4.0 days, masses of 0.36 to 1.45…”

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confidence: 99%

Transiting extrasolar planetary candidates in the Galactic bulge

Sahu

Casertano

Bond

et al. 2006

Nature

150

180

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Radial-velocity (RV) searches 1-3 have led to the unanticipated discovery of Jovian-mass exoplanets with orbital periods of only a few days---"hot Jupiters." RV surveys favor stars bright enough for high-resolution spectroscopy, and have thus generally been limited to nearby stars that are hotter than early K spectral type, although RV studies are now being extended to M dwarfs [4][5] . Photometric monitoring of microlensing events provides another technique that has recently led to the discovery of a 5.5 Earth-mass planet around a low-mass star 6 .The increasingly successful transit surveys are based on detecting the recurrent dimming of the primary star caused by the silhouetted planet transiting across its face. The first transiting planet, HD 209458b, was found through photometric follow-up of a RV detection [7][8] . Subsequently, five of the transiting candidates found by the OGLE survey 9 have been confirmed as having planetary masses through RV measurements [10][11][12][13][14] , and four other planets around bright field stars have been found in separate transit surveys [15][16][17][18] . These ten RVconfirmed transiting planets have periods between 1.2 and 4.0 days, masses of 0.36 to 1.45

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“…Theoretically, a similar degree of variability is expected to be discovered in the future exploration of extra-solar systems. Although today the direct exploration of exoplanets is well beyond the capabilities of science, their existence has been confirmed recently (i.e., Mayor and Queloz 1995;Lissauer 1999;Throop et al 2001;Ford et al 2001;Konacki et al 2003).…”

Section: Exoplanetsmentioning

confidence: 99%

Extraterrestrial hydrogeology

et al. 2005

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Subsurface water processes are common for planetary bodies in the solar system and are highly probable for exoplanets (planets outside the solar system). For many solar system objects, the subsurface water exists as ice. For Earth and Mars, subsurface saturated zones have occurred throughout their planetary histories. Earth is mostly clement with the recharge of most groundwater reservoirs from ample precipitation during transient iceand hot-house conditions, as recorded through the geologic and fossilized records. On the other hand, Mars is mostly in an ice-house stage, which is interrupted by endogenic-driven activity. This activity catastrophically drives short-lived hydrological cycling and associated climatic perturbations. Regional aquifers in the Martian highlands that developed during past, more Earth-like conditions delivered water to the northern plains. Water was also cycled to the South Polar Region during changes in climate induced by endogenic activity and/or by changes in Mars' orbital parameters. Venus very likely had a warm hydrosphere for hundreds of millions of years, before the development of its current extremely hot atmosphere and surface. Subsequently, Venus lost its hydrosphere as solar luminosity increased and a run-away moist greenhouse took effect. Subsurface oceans of water or ammonia-water composition, induced by tidal forces and radiogenic heating, probably occur on the larger satellites Europa, Ganymede, Callisto, Titan, and Triton. Tidal forces operating between some of the small bodies of the outer solar system could also promote the fusion of ice and the stability of inner liquid-water oceans.RØsumØ Les processus de subsurface impliquant l'eau sont communs pour les corps planØtaires du syst me solaire et sont tr s probables sur les exoplan tes (plan tes en dehors du syst me solaire). Pour plusieurs objets du syst mes solaire, l'eau de subsurface est prØsente sous forme de glace. Pour la Terre et Mars, les zones saturØes de subsurface apparaissent à travers toute leur histoire planØtaire. La Terre est particuli rement clØmente avec la recharge des rØservoirs, avec de amples prØcipitations, des conditions glaciaires et de fortes chaleurs, comme l'atteste les enregistrements gØologiques et palØontologiques. D'un autre côtØ, Mars se trouve dans une phase essentiellement glaciaire, qui est interrompue par des activitØs contraintes par les phØnom nes endogØniques. Cette activitØ conduit de mani re catastrophique à des cycles hydrologiques et à des perturbations climatiques brutaux. Les aquif res rØgionaux dans les haute terres martiennes qui se sont formØs dans des conditions similaires aux conditions terrestres, alimentent les plaines du Nord. Resumen Los procesos hídricos subsuperficiales son comunes en cuerpos planetarios del sistema solar y son altamente probables para exoplanetas (planetas fuera del sistema solar). Para muchos cuerpos del sistema solar, el agua subsuperficial existe como hielo. Para la Tierra y Marte han ocurrido zonas saturadas subsuperficiales a travØ...

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An extrasolar planet that transits the disk of its parent star

Cited by 303 publications

References 16 publications

Millimagnitude photometry for transiting extrasolar planetary candidates

Millimagnitude photometry for transiting extrasolar planetary candidates

Transiting extrasolar planetary candidates in the Galactic bulge

Extraterrestrial hydrogeology

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