Sentences with phrase «orbital radii of»

«This is the widest range of orbital radii of any planetary system known,» Marois told New Scientist.

For an object so big, these flashes are extremely short, implying a radiating surface about the same as a sphere with orbital radius of Jupiter.

The emission fits a model with a grain temperature of 40 K, indicating a minimum orbital radius of 60 AU from the host star.

The radius corresponds to 10 times the orbital radius of Neptune in our solar system.

Not exact matches

Orbital radius of such star should be about 33 astronomical units, the orbital length should then exceed two hundred astronomical units.»

They eliminated those with orbital radii less than one tenth that of Earth's, because at that distance moon systems might not remain in stable orbits around their planets on billion - year timescales.

Their models showed that if you visited any star with a planet orbiting from the same distance as Earth down to one tenth that, there is about a 38 percent chance (and likely less) that you would run into a planet and moon system similar to Jupiter's four Galilean satellites (Io, Europa, Ganymede and Callisto), with similar ratios of moon to planetary diameters and orbital to planetary radii.

The planet is extremely close to its star — its orbital radius is only about three times the radius of the star — and the scientists have estimated that its surface temperatures may be as high as 3,000 degrees Kelvin, or more than 5,000 degrees Fahrenheit.

This chart shows, on the top row, artist concepts of the seven planets of TRAPPIST - 1 with their orbital periods, distances from their star, radii and masses as compared to those of Earth.

A simulation (Wolf & D'Angelo 2005) of ALMA observations at 950 GHz of a disc shows an embedded protoplanet of 1 Jupiter Mass around a 0.5 Solar Mass star (orbital radius: 5AU).

A subsequent analysis using the most recent kinematic and radial velocity data available in the literature, however, found Proxima «is quitely likely» to be bound to to Stars A and B based on calculations of the binding energy of Proxima relative to the center of mass of the entire triple system, where its orbital semi-major axis exceeds 10,000 AUs and is «on order the same size as Alpha Centauri AB's Hill radius in the galactic potential» (Wertheimer and Laughlin, 2006).

Through ACCESS, we are compiling a library of exoplanet transmission spectra, which will ultimately enable us and the wider exoplanet atmosphere community to study trends in the atmospheric properties of exoplanets as they relate to the exoplanets» masses, radii, and orbital parameters.

On the other hand, stars Aa and Ab have are separated by only 3.76 solar radii, which is about 14.9 times the radius of CM Draconis Aa (Claud H. Lacy, 1977), and have a mutual orbital period of just under 1.27 days (Deeg et al, 1998; Metcalfe et al, 1996; and Claud H. Lacy, 1977).

Our new -LCB- \ em Spitzer -RCB- observations were taken two years after the original K2 discovery data and have a significantly higher cadence, allowing us to derive improved estimates for this planet's radius, semi-major axis, and orbital period, which greatly reduce the uncertainty in the prediction of near future transit times for the -LCB- \ em James Webb Space Telescope -RCB--LRB--LCB- \ em JWST -RCB--RRB- observations.

This study examines planet occurrence rates for the Kepler GK dwarf target sample for planet radii, 0.75 < Rp < 2.5 Rearth, and orbital periods, 50 < Porb < 300 days, with an emphasis on a thorough exploration and identification of the most important sources of systematic uncertainties.

We find that 16.5 + / - 3.6 % of main - sequence FGK stars have at least one planet between 0.8 and 1.25 Earth radii with orbital periods up to 85 days.

Based on the star's mass and the period of the shift, we can also calculate the planet's orbital radius.

Results from just forty - three days of data along with ground - based follow - up observations have identified five new transiting planets with measurements of their masses, radii, and orbital periods.

Detailed modeling of the transit is consistent with a planetary companion with an orbital period of 3.548460 + / -0.000032 days and a radius of 1.431 + / -0.050 Rj.

Multiple planets transiting the same star reveal more: period ratios determine stability and dynamics, mutual gravitational interactions reflect planet masses and orbital shapes, and the fraction of transiting planets obs... ▽ More When an extrasolar planet passes in front of its star (transits), its radius can be measured from the decrease in starlight and its orbital period from the time between transits.

Abstract: When an extrasolar planet passes in front of its star (transits), its radius can be measured from the decrease in starlight and its orbital period from the time between transits.

They examined how the orbital distances of their final sample are related to the planetary mass and / or the planetary radius, depending on which measurements are available.

Indeed, stable orbits may extend as far as one third of the closest separation between any two stars in a binary system, but according to NASA's Kepler Mission team, numerical integration models have shown that there is a range of orbital radii between about 1/3 and 3.5 times the stellar separation for which stable orbits around two stars are not possible (Holman and Wiegert, 1999; Wiegert and Holman, 1997; and Donnison and Mikulskis, 1992).