Extra-solar planets
... orbits the Sun (0.39 AU). While the Doppler technique preferentially selects systems in tight orbits, giant planets so close to the parent star were generally unexpected. Theoretical progress in understanding their formation and their properties has been rapid, but it remains far from complete. ‡ Ba ...
... orbits the Sun (0.39 AU). While the Doppler technique preferentially selects systems in tight orbits, giant planets so close to the parent star were generally unexpected. Theoretical progress in understanding their formation and their properties has been rapid, but it remains far from complete. ‡ Ba ...
Characterization of exoplanetary systems with the direct
... In the year of the 20th anniversary of the discovery of the first extrasolar planet we can count more than 1800 companions found with different techniques. The majority of them are indirect methods that infer the presence of an orbiting body by observing the parent star (radial velocity, transits, a ...
... In the year of the 20th anniversary of the discovery of the first extrasolar planet we can count more than 1800 companions found with different techniques. The majority of them are indirect methods that infer the presence of an orbiting body by observing the parent star (radial velocity, transits, a ...
A Decade of Radial-Velocity Discoveries in the Exoplanet Domain
... Younger primary stars among them, less amenable to radial-velocity searches because of the intrinsic astrophysical noise of the star, will be suitable targets for direct imaging searches (see the chapter by Beuzit et al.). Lower-mass planets could exist on long-period orbits as well; however, these ...
... Younger primary stars among them, less amenable to radial-velocity searches because of the intrinsic astrophysical noise of the star, will be suitable targets for direct imaging searches (see the chapter by Beuzit et al.). Lower-mass planets could exist on long-period orbits as well; however, these ...
Extra-solar planets
... expected. More than one-third have significantly elliptical orbits, with e > 0.3, compared with the largest eccentricities in our solar system, of about 0.2 for Mercury and Pluto and 0.05 for Jupiter. Even more significantly, about two-thirds are orbiting their host star much closer than Mercury orb ...
... expected. More than one-third have significantly elliptical orbits, with e > 0.3, compared with the largest eccentricities in our solar system, of about 0.2 for Mercury and Pluto and 0.05 for Jupiter. Even more significantly, about two-thirds are orbiting their host star much closer than Mercury orb ...
148 Jun - British Astronomical Association
... Maxima values have a mean magnitude of 7.2, varying in extreme from 6.8 to 8.4. Minima had a mean of 10.0, and varying mainly from 9.0 to 11.4 magnitude. From JD 2447700 for about 3 years (not shown in these plots) there is an interval of irregular changes about 1.2 magnitude in amplitude. ...
... Maxima values have a mean magnitude of 7.2, varying in extreme from 6.8 to 8.4. Minima had a mean of 10.0, and varying mainly from 9.0 to 11.4 magnitude. From JD 2447700 for about 3 years (not shown in these plots) there is an interval of irregular changes about 1.2 magnitude in amplitude. ...
The HARPS search for southern extra-solar planets
... characterize planets in the super-Earth and Neptune mass regime. Methods. The size of our star sample and the precision achieved with HARPS have allowed the detection of a sufficiently large number of low-mass planets to study the statistical properties of their orbital elements, the correlation of ...
... characterize planets in the super-Earth and Neptune mass regime. Methods. The size of our star sample and the precision achieved with HARPS have allowed the detection of a sufficiently large number of low-mass planets to study the statistical properties of their orbital elements, the correlation of ...
Exoplanetary Geophysics-
... motion projected onto the plane of the sky. This so-called astrometric technique is most sensitive to massive planets orbiting stars that are relatively close to Earth. Because the star’s motion is detectable in two dimensions, the planet’s actual mass, rather than just the combination M sin i, can ...
... motion projected onto the plane of the sky. This so-called astrometric technique is most sensitive to massive planets orbiting stars that are relatively close to Earth. Because the star’s motion is detectable in two dimensions, the planet’s actual mass, rather than just the combination M sin i, can ...
Exoplanet Detection Techniques - Lunar and Planetary Laboratory
... The high fraction of Earth-size planets estimated to orbit in the habitable zones (HZs) of M dwarfs (Dressing and Charbonneau, 2013; Kopparapu, 2013; Bonfils et al., 2013) makes the low mass stars very attractive targets for Doppler RV surveys. The lower stellar mass of the M dwarfs, as well as the ...
... The high fraction of Earth-size planets estimated to orbit in the habitable zones (HZs) of M dwarfs (Dressing and Charbonneau, 2013; Kopparapu, 2013; Bonfils et al., 2013) makes the low mass stars very attractive targets for Doppler RV surveys. The lower stellar mass of the M dwarfs, as well as the ...
Detecting Exoplanets Talk
... of last month was about the same as radial velocity. • With new space missions, transits may pop into the lead. • Other methods are less important by comparison. 2010 Sept 10 ...
... of last month was about the same as radial velocity. • With new space missions, transits may pop into the lead. • Other methods are less important by comparison. 2010 Sept 10 ...
Abstracts for “Extreme Solar Systems” Talk Abstracts “Pulsar Planets
... In the last twelve years, more than 200 exoplanets have been detected. These discoveries have revealed the impressive diversity of exoplanet orbital properties. The past twelve years have also witnessed a remarkable improvement of the precision of radial velocity measurements with a gain of about a ...
... In the last twelve years, more than 200 exoplanets have been detected. These discoveries have revealed the impressive diversity of exoplanet orbital properties. The past twelve years have also witnessed a remarkable improvement of the precision of radial velocity measurements with a gain of about a ...
1 Exoplanet Observations - Wiley-VCH
... data from recent discoveries and its statistics are consistent with the results from volume-limited [15] and magnitude-limited [16] surveys. We include only objects with 0.3MJup < M < 20MJup and which were discovered from radial velocity surveys. The considered sample size is 204 exoplanets. We use ...
... data from recent discoveries and its statistics are consistent with the results from volume-limited [15] and magnitude-limited [16] surveys. We include only objects with 0.3MJup < M < 20MJup and which were discovered from radial velocity surveys. The considered sample size is 204 exoplanets. We use ...
Investigation of Extrasolar Planets Using Radial Velocity Technique
... This was a rather strange discovery because it was revolving around a pulsar rather than a main sequence star like the Sun [14]. It is worth mentioning, pulsars are different from the Sun and any planets orbiting them would not be expected to harbor life as in the solar system [12]. The first discov ...
... This was a rather strange discovery because it was revolving around a pulsar rather than a main sequence star like the Sun [14]. It is worth mentioning, pulsars are different from the Sun and any planets orbiting them would not be expected to harbor life as in the solar system [12]. The first discov ...
Extrasolar Planet Orbits and Eccentricities
... planets are ejected from the system when they reach e = 1, there is also a boundary condition n(1,t) = 0. We assume that the diffusion coefficient is a power law, D(e) ∝ e p . The best-fit ccentricity distributions that emerge from the diffusion models are plotted in Figure 3. They are shown at late ...
... planets are ejected from the system when they reach e = 1, there is also a boundary condition n(1,t) = 0. We assume that the diffusion coefficient is a power law, D(e) ∝ e p . The best-fit ccentricity distributions that emerge from the diffusion models are plotted in Figure 3. They are shown at late ...
Extra-solar planets: detection methods and results
... properties (e.g. Udry et al., 2003), as well as of their host stars (Gonzalez, 1998; Santos et al., 2004c). These studies are providing the first constraints on the physical and chemical processes involved in the formation of these systems. It is now known that planets can form far from their host st ...
... properties (e.g. Udry et al., 2003), as well as of their host stars (Gonzalez, 1998; Santos et al., 2004c). These studies are providing the first constraints on the physical and chemical processes involved in the formation of these systems. It is now known that planets can form far from their host st ...
The spectral characteristics of transiting extrasolar planet Jae
... be 13 m/s with a period of 12 years for the Jupiter and 0.089 m/s for the Earth during 1 year. This means that long-term observation is required for confirmation of exoplanet with broad orbital separation, and this fact means that exoplanets detected by the RV method mostly have short periods (a day ...
... be 13 m/s with a period of 12 years for the Jupiter and 0.089 m/s for the Earth during 1 year. This means that long-term observation is required for confirmation of exoplanet with broad orbital separation, and this fact means that exoplanets detected by the RV method mostly have short periods (a day ...
Direct Imaging of Radial Velocity Exoplanets
... information about the planet including its atmospheric composition. When the light of the star passes the planet, the planet’s atmosphere will absorb the light at different degrees. Based on this information, the absorption spectrum of the planet can be created from which the presence of different g ...
... information about the planet including its atmospheric composition. When the light of the star passes the planet, the planet’s atmosphere will absorb the light at different degrees. Based on this information, the absorption spectrum of the planet can be created from which the presence of different g ...
minimum mass extrasolar nebula derived from the
... The distibution of the planets can bee seen from Figures 3.1- 3.2 from which we conclude that the mean host temperature is approximately between 4500K and 6300K. For comparison the Sun has an effective temperature of about 5777K. Yet, the surface density profiles show 3.3- 3.5 that the Solar system ...
... The distibution of the planets can bee seen from Figures 3.1- 3.2 from which we conclude that the mean host temperature is approximately between 4500K and 6300K. For comparison the Sun has an effective temperature of about 5777K. Yet, the surface density profiles show 3.3- 3.5 that the Solar system ...
Doppler spectroscopy as a path to the detection of Earth
... seems difficult to form a massive planet in such a metal-poor environment11 (see ‘Chemical clues for stars with planets’). For instance, a recent high-precision 10-year-survey of more than 100 solar-type stars has not revealed one single gas-giant planet with metallicity significantly lower than −0. ...
... seems difficult to form a massive planet in such a metal-poor environment11 (see ‘Chemical clues for stars with planets’). For instance, a recent high-precision 10-year-survey of more than 100 solar-type stars has not revealed one single gas-giant planet with metallicity significantly lower than −0. ...
2 The Diversity of Extrasolar Planets Around Solar Type Stars
... to the planet search, this sample will allow us to collect information on spectroscopic binaries and give us a synthetic view on companions to solar type stars from q=m2/m1=1 down to q ≤ 0.001. On April 4th 2001 [18], we announced the latest results related to these two programs, namely the detectio ...
... to the planet search, this sample will allow us to collect information on spectroscopic binaries and give us a synthetic view on companions to solar type stars from q=m2/m1=1 down to q ≤ 0.001. On April 4th 2001 [18], we announced the latest results related to these two programs, namely the detectio ...
ph507-16-1exo3
... 0. About 15% have an eccentricity smaller than Earth's, and over 25% have an eccentricity smaller than Jupiter's. 45% are smaller than Mercury's eccentricity, and 50% are lower than Pluto's. Planets within 0.1 AU are presumably tidally circularized. Note that the distance of closest approach is a(1- ...
... 0. About 15% have an eccentricity smaller than Earth's, and over 25% have an eccentricity smaller than Jupiter's. 45% are smaller than Mercury's eccentricity, and 50% are lower than Pluto's. Planets within 0.1 AU are presumably tidally circularized. Note that the distance of closest approach is a(1- ...
From Hot Jupiters to Hot Neptunes and Below
... largest amplitudes (up to 10 m s−1 peak-to-peak) whereas late-K dwarfs show only weak modulations (1–2 m s−1 ). Periods also vary along the main sequence, ranging from ∼4 to ∼15 minutes between K and early-G stars. These RV measurements have an accuracy better than 40 cm s−1 (including photon noise ...
... largest amplitudes (up to 10 m s−1 peak-to-peak) whereas late-K dwarfs show only weak modulations (1–2 m s−1 ). Periods also vary along the main sequence, ranging from ∼4 to ∼15 minutes between K and early-G stars. These RV measurements have an accuracy better than 40 cm s−1 (including photon noise ...
Presentation
... “But if GJ 581g is confirmed by further RV scrutiny, the mere fact that a habitable planet has been detected this soon, around such a nearby star, suggests that [the fraction of stars with potentially habitable planets] could well be on the order of a few tens of percent, and thus that either we hav ...
... “But if GJ 581g is confirmed by further RV scrutiny, the mere fact that a habitable planet has been detected this soon, around such a nearby star, suggests that [the fraction of stars with potentially habitable planets] could well be on the order of a few tens of percent, and thus that either we hav ...
Resource Letter Exo
... many more expected from the ongoing Kepler satellite analysis). The architecture of many of the systems (in terms of masses and orbits) are qualitatively different than those that had been expected on the basis of our own solar system. Explaining their properties has led to a substantial advance in ...
... many more expected from the ongoing Kepler satellite analysis). The architecture of many of the systems (in terms of masses and orbits) are qualitatively different than those that had been expected on the basis of our own solar system. Explaining their properties has led to a substantial advance in ...
Tau Ceti
Tau Ceti (τ Cet, τ Ceti) is a star in the constellation Cetus that is spectrally similar to the Sun, although it has only about 78% of the Sun's mass. At a distance of just under 12 light-years from the Solar System, it is a relatively nearby star, and is the closest solitary G-class star. The star appears stable, with little stellar variation, and is metal-deficient.Observations have detected more than ten times as much dust surrounding Tau Ceti as is present in the Solar System. Since December 2012, there has been evidence of possibly five planets orbiting Tau Ceti, with two of these being potentially in the habitable zone. Because of its debris disk, any planet orbiting Tau Ceti would face far more impact events than Earth. Despite this hurdle to habitability, its solar analog (Sun-like) characteristics have led to widespread interest in the star. Given its stability, similarity and relative proximity to the Sun, Tau Ceti is consistently listed as a target for the Search for Extra-Terrestrial Intelligence (SETI), and it appears in some science fiction literature.It can be seen with the unaided eye as a third-magnitude star. As seen from Tau Ceti, the Sun would be a third-magnitude star in the constellation Boötes.