Discovery and spectroscopy of the young Jovian planet
... hints about their formation. Several unexpected results have emerged. The near-infrared colors of these planets are mostly red, indicating cloudy atmospheres reminiscent of brown dwarfs of spectral type L. Methane absorption features are prominent in the near-infrared spectra of T dwarfs (Teff <1100 ...
... hints about their formation. Several unexpected results have emerged. The near-infrared colors of these planets are mostly red, indicating cloudy atmospheres reminiscent of brown dwarfs of spectral type L. Methane absorption features are prominent in the near-infrared spectra of T dwarfs (Teff <1100 ...
A STEP - Observatoire de la Côte d`Azur
... Fig XXX - Comparison of detection threshold with “white noise” (blue line), which does not undergo temporal correlation and detection limit with “red noise” (linked to systematic effects - green line) – The pink to red part of the diagram shows the density of Hot Jupiter planets at given transit dep ...
... Fig XXX - Comparison of detection threshold with “white noise” (blue line), which does not undergo temporal correlation and detection limit with “red noise” (linked to systematic effects - green line) – The pink to red part of the diagram shows the density of Hot Jupiter planets at given transit dep ...
Why was Pluto once considered a planet?
... • There may be 100,000 TNOs larger than 100 km, and the total mass may be ~0.01 ME. ...
... • There may be 100,000 TNOs larger than 100 km, and the total mass may be ~0.01 ME. ...
Extrasolar Cosmochemistry
... loss is relatively slow in the sense that it takes much longer than an asteroid’s orbital period. As a consequence, the asteroid’s angular momentum is approximately conserved, and it migrates outward but is still gravitationally bound (Duncan & Lissauer 1998). If initially further than 2.5 AU (AU = ...
... loss is relatively slow in the sense that it takes much longer than an asteroid’s orbital period. As a consequence, the asteroid’s angular momentum is approximately conserved, and it migrates outward but is still gravitationally bound (Duncan & Lissauer 1998). If initially further than 2.5 AU (AU = ...
- ANU Repository
... is flat except for a decline for orbits less than a few days. 12 candidate planets, including two Jupiter-size objects, experience an irradiance below the threshold level for a runaway greenhouse on an Earth-like planet and are thus in a ‘habitable zone’. Key words: stars: abundances – stars: fundame ...
... is flat except for a decline for orbits less than a few days. 12 candidate planets, including two Jupiter-size objects, experience an irradiance below the threshold level for a runaway greenhouse on an Earth-like planet and are thus in a ‘habitable zone’. Key words: stars: abundances – stars: fundame ...
November, 2015 - The Baton Rouge Astronomical Society
... Angeles. “Any theoretical or computational models have to explain what we actually find.” One big early surprise (1995) was the ground-based discovery of “hot Jupiters:” gas giants the size of Jupiter in orbits around their parent stars much closer than Venus—or even Mercury—is to the Sun. How does ...
... Angeles. “Any theoretical or computational models have to explain what we actually find.” One big early surprise (1995) was the ground-based discovery of “hot Jupiters:” gas giants the size of Jupiter in orbits around their parent stars much closer than Venus—or even Mercury—is to the Sun. How does ...
Tidal Venuses: Triggering a Climate Catastrophe via Tidal Heating
... i.e. one hemisphere always facing the star, was emphasized. Kasting et al. (1993) quantified this concept and found that planets orbiting within the HZ of stars less than two-thirds the mass of the Sun were in danger of synchronization. Although their analysis was limited to Earth-like planets on ci ...
... i.e. one hemisphere always facing the star, was emphasized. Kasting et al. (1993) quantified this concept and found that planets orbiting within the HZ of stars less than two-thirds the mass of the Sun were in danger of synchronization. Although their analysis was limited to Earth-like planets on ci ...
Effect of the stellar spin history on the tidal evolution of close
... Methods. We used a standard equilibrium tidal model to compute the orbital evolution of single planets orbiting both Sun-like stars and very low-mass stars (0.1 M ). We tested two stellar spin evolution profiles, one with fast initial rotation (1.2 day rotation period) and one with slow initial rot ...
... Methods. We used a standard equilibrium tidal model to compute the orbital evolution of single planets orbiting both Sun-like stars and very low-mass stars (0.1 M ). We tested two stellar spin evolution profiles, one with fast initial rotation (1.2 day rotation period) and one with slow initial rot ...
Solar System
... could not grow very large. The giant planets (Jupiter, Saturn, Uranus, and Neptune) formed further out, be- 4 Sun yond the frost line, the point between the orbits of Mars and Jupiter where material is cool enough for volatile icy Main article: Sun compounds to remain solid. The ices that formed the ...
... could not grow very large. The giant planets (Jupiter, Saturn, Uranus, and Neptune) formed further out, be- 4 Sun yond the frost line, the point between the orbits of Mars and Jupiter where material is cool enough for volatile icy Main article: Sun compounds to remain solid. The ices that formed the ...
Phase light curves for extrasolar Jupiter and Saturn
... instruments from the ground (Collier-Cameron references) and space (MOST references) are capable of detecting variations of the order 10−4 − 10−6 of the total star light (Jenkins & Doyle 2003; Green et al. 2003), at the limit of what might be expected from the class of ”hot Jupiter” planets, i. e., ...
... instruments from the ground (Collier-Cameron references) and space (MOST references) are capable of detecting variations of the order 10−4 − 10−6 of the total star light (Jenkins & Doyle 2003; Green et al. 2003), at the limit of what might be expected from the class of ”hot Jupiter” planets, i. e., ...
Life Beyond Earth Exhibition
... exhibits housed in the Our Place In Space area of the building. Major sections of the exhibition cover the vastness of the universe, places in the solar system where life could exist, the search for exoplanets, and questions that remain to be answered. The exhibit includes several iconic elements. A ...
... exhibits housed in the Our Place In Space area of the building. Major sections of the exhibition cover the vastness of the universe, places in the solar system where life could exist, the search for exoplanets, and questions that remain to be answered. The exhibit includes several iconic elements. A ...
Constraints on Long-Period Planets from an L
... method. The limited temporal baseline of radial velocity observations, and the need to observe for a complete orbital period to confirm the properties of a planet with confidence, currently limit RV planets to periods of about 10 years or less (Cumming et al. 2008; Butler et al. 2006). The masses of ...
... method. The limited temporal baseline of radial velocity observations, and the need to observe for a complete orbital period to confirm the properties of a planet with confidence, currently limit RV planets to periods of about 10 years or less (Cumming et al. 2008; Butler et al. 2006). The masses of ...
Radial Velocity - Yale Exoplanet
... achieved the unprecedented precision of 15 m s−1 . Unfortunately, because of the small sample size, no planets were found. However, upper limits were set on M sin i for orbital periods out to 15 years for the 21 stars that they observed (Walker et al. 1995). Cross-correlation speedometers were also ...
... achieved the unprecedented precision of 15 m s−1 . Unfortunately, because of the small sample size, no planets were found. However, upper limits were set on M sin i for orbital periods out to 15 years for the 21 stars that they observed (Walker et al. 1995). Cross-correlation speedometers were also ...
The Neptune Trojans: a window on the birth of the solar system
... orbital stability located 60° ahead and behind the planet in its orbit, respectively), orbiting the Sun with periods approximately equal to that of the giant planet. Any that leave the Trojan clouds (perhaps nudged through collisions, or perturbed by the distant gravitational influence of other plan ...
... orbital stability located 60° ahead and behind the planet in its orbit, respectively), orbiting the Sun with periods approximately equal to that of the giant planet. Any that leave the Trojan clouds (perhaps nudged through collisions, or perturbed by the distant gravitational influence of other plan ...
Lecture26_Future
... Arthur Clarke: “Sometimes I think we’re alone in the universe, and sometimes I think we’re not. In either case, the idea is quite staggering.” ...
... Arthur Clarke: “Sometimes I think we’re alone in the universe, and sometimes I think we’re not. In either case, the idea is quite staggering.” ...
Dynamical evolution of planetary systems
... There are two possible mechanisms by which we envision that giant planets can form. The first is nicknamed the “core-accretion mechanism”: the coagulation of solid particles forms a core typically of about 10 Earth masses (M⊕ ) while the gas is still present in the proto-planetary disk; the core the ...
... There are two possible mechanisms by which we envision that giant planets can form. The first is nicknamed the “core-accretion mechanism”: the coagulation of solid particles forms a core typically of about 10 Earth masses (M⊕ ) while the gas is still present in the proto-planetary disk; the core the ...
Looking for planets with SPHERE in planetary systems with double
... Debris disks are optically thin, almost gas-free dusty disks observed around a significant fraction of main-sequence stars older than about 10 Myr. Since the circumstellar dust is short-lived, the very existence of these disks is considered as an evidence that dust-producing planetesimals are still ...
... Debris disks are optically thin, almost gas-free dusty disks observed around a significant fraction of main-sequence stars older than about 10 Myr. Since the circumstellar dust is short-lived, the very existence of these disks is considered as an evidence that dust-producing planetesimals are still ...
10. Atmospheres of Planets and of Exoplanets - ETH E
... So far it was a riddle: How is it possible that the low-mass intermost and hottest Planet can keep a permant Atmosphere, even though this Atmosphere is extremely thin? On the day side, the surface temperature of Mercury is over 400oC (s. p. 419). Due to the strong radiation of the Sun, the component ...
... So far it was a riddle: How is it possible that the low-mass intermost and hottest Planet can keep a permant Atmosphere, even though this Atmosphere is extremely thin? On the day side, the surface temperature of Mercury is over 400oC (s. p. 419). Due to the strong radiation of the Sun, the component ...
Habitable Zone Lifetimes of Exoplanets around Main Sequence Stars
... Lammer et al., 2009). The existence of liquid water also requires planetary temperatures to be within the range expected to be optimal for life. 1.1. On the definition of the ‘‘habitable zone’’ Throughout this paper, we use the seminal HZ study of Kasting et al. (1993) and the Selsis et al. (2007) e ...
... Lammer et al., 2009). The existence of liquid water also requires planetary temperatures to be within the range expected to be optimal for life. 1.1. On the definition of the ‘‘habitable zone’’ Throughout this paper, we use the seminal HZ study of Kasting et al. (1993) and the Selsis et al. (2007) e ...
Extrasolar planets - Astronomisk Ungdom
... As mentioned above a macula can disappear and reappear. However, planets do not vanish from their orbit without a trace or a caveat, except if it is a free planet passing the star, but those are rare and not yet accurately proven. All work around extra solar planets is fairly new and current. At pre ...
... As mentioned above a macula can disappear and reappear. However, planets do not vanish from their orbit without a trace or a caveat, except if it is a free planet passing the star, but those are rare and not yet accurately proven. All work around extra solar planets is fairly new and current. At pre ...
MEarth
... dwarfs. Firstly, the growing number of M-dwarf exoplanet discoveries, including the ∼5:5 M ⊕ planet orbiting Gliese 581c (Udry et al. 2007) and the microlensing discovery OGLE 2005-BLG-390Lb (Beaulieu et al. 2006), suggest an abundance of sub-Neptune mass planets orbiting M dwarfs. It is an open c ...
... dwarfs. Firstly, the growing number of M-dwarf exoplanet discoveries, including the ∼5:5 M ⊕ planet orbiting Gliese 581c (Udry et al. 2007) and the microlensing discovery OGLE 2005-BLG-390Lb (Beaulieu et al. 2006), suggest an abundance of sub-Neptune mass planets orbiting M dwarfs. It is an open c ...
The Habitability of Planets Orbiting M
... orbiting other stars1 . Many of these planets are especially captivating because of their orbital distances, which place them in their stars’ canonical habitable zone—the region around a star where an orbiting planet with an Earth-like atmosphere (CO2 -H2 O-N2 ) could maintain water in liquid form o ...
... orbiting other stars1 . Many of these planets are especially captivating because of their orbital distances, which place them in their stars’ canonical habitable zone—the region around a star where an orbiting planet with an Earth-like atmosphere (CO2 -H2 O-N2 ) could maintain water in liquid form o ...
CHEOPS Science Requirements Document
... at any time. Furthermore, planetary orbits were thought to be well aligned with the star’s equator (Fabrycky & Winn 2009), resulting from the notion of disc-driven migration (Lin et al. 1996; Ward 1997). Surprisingly, hot-Jupiter planets on non-coplanar orbits appear to be more common than previousl ...
... at any time. Furthermore, planetary orbits were thought to be well aligned with the star’s equator (Fabrycky & Winn 2009), resulting from the notion of disc-driven migration (Lin et al. 1996; Ward 1997). Surprisingly, hot-Jupiter planets on non-coplanar orbits appear to be more common than previousl ...
ISNS3371_041007_bw
... • We finally obtained direct evidence of the existence of an extrasolar planet in the year 1995. – A planet was discovered in orbit around the star 51 Pegasi. – Over 100 such extrasolar planets are now known to exist. ...
... • We finally obtained direct evidence of the existence of an extrasolar planet in the year 1995. – A planet was discovered in orbit around the star 51 Pegasi. – Over 100 such extrasolar planets are now known to exist. ...
Planet
A planet (from Ancient Greek ἀστήρ πλανήτης (astēr planētēs), or πλάνης ἀστήρ (plánēs astēr), meaning ""wandering star"") is an astronomical object orbiting a star, brown dwarf, or stellar remnant that is massive enough to be rounded by its own gravity, is not massive enough to cause thermonuclear fusion, and has cleared its neighbouring region of planetesimals.The term planet is ancient, with ties to history, science, mythology, and religion. Several planets in the Solar System can be seen with the naked eye. These were regarded by many early cultures as divine, or as emissaries of deities. As scientific knowledge advanced, human perception of the planets changed, incorporating a number of disparate objects. In 2006, the International Astronomical Union (IAU) officially adopted a resolution defining planets within the Solar System. This definition is controversial because it excludes many objects of planetary mass based on where or what they orbit. Although eight of the planetary bodies discovered before 1950 remain ""planets"" under the modern definition, some celestial bodies, such as Ceres, Pallas, Juno, Vesta (each an object in the solar asteroid belt), and Pluto (the first trans-Neptunian object discovered), that were once considered planets by the scientific community are no longer viewed as such.The planets were thought by Ptolemy to orbit Earth in deferent and epicycle motions. Although the idea that the planets orbited the Sun had been suggested many times, it was not until the 17th century that this view was supported by evidence from the first telescopic astronomical observations, performed by Galileo Galilei. By careful analysis of the observation data, Johannes Kepler found the planets' orbits were not circular but elliptical. As observational tools improved, astronomers saw that, like Earth, the planets rotated around tilted axes, and some shared such features as ice caps and seasons. Since the dawn of the Space Age, close observation by space probes has found that Earth and the other planets share characteristics such as volcanism, hurricanes, tectonics, and even hydrology.Planets are generally divided into two main types: large low-density giant planets, and smaller rocky terrestrials. Under IAU definitions, there are eight planets in the Solar System. In order of increasing distance from the Sun, they are the four terrestrials, Mercury, Venus, Earth, and Mars, then the four giant planets, Jupiter, Saturn, Uranus, and Neptune. Six of the planets are orbited by one or more natural satellites.More than a thousand planets around other stars (""extrasolar planets"" or ""exoplanets"") have been discovered in the Milky Way: as of 1 October 2015, 1968 known extrasolar planets in 1248 planetary systems (including 490 multiple planetary systems), ranging in size from just above the size of the Moon to gas giants about twice as large as Jupiter. On December 20, 2011, the Kepler Space Telescope team reported the discovery of the first Earth-sized extrasolar planets, Kepler-20e and Kepler-20f, orbiting a Sun-like star, Kepler-20. A 2012 study, analyzing gravitational microlensing data, estimates an average of at least 1.6 bound planets for every star in the Milky Way.Around one in five Sun-like stars is thought to have an Earth-sized planet in its habitable zone.