Sentences with phrase «heavier than hydrogen»

On July 21, 2003, some astronomers provided evidence from recent discoveries of giant extrasolar planets in mostly inner orbits around host stars that planetary systems may be more common around stars whose spectra show an enriched abundance of elements heavier than hydrogen and helium — also called high «metallicity» (exoplanets.org press release; and Gonzalez, 1999).

It may be 105 to to 112 percent as enriched as Sol with elements heavier than hydrogen («metallicity»), based on its abundance of iron (Porto de Mello and da Silva, 1997; and Cayrel de Strobel et al, 1991, 300).

Second generation stars do not just burn hydrogen, they also burn heavier elements, like helium and metals (elements heavier than hydrogen and helium), and were formed from supernova explosions (the debris of exploded population II stars).

The star may have only around 81 percent of Sol's abundance of elements heavier than hydrogen — «metallicity» (Ansgar Reiners, 2007, from Jenkins et al, 2009).

It appears to be only around 44 percent as enriched as Sol with elements heavier than hydrogen («metallicity»), based on its abundance of iron.

Since 1990, it has been measured to be around 85 to 155 percent as enriched as Sol with elements heavier than hydrogen («metallicity»), based on its abundance of iron (Hatzes et al, 2006; and Drake and Smith, 1990).

Stars and galaxies 12.9 billion light - years away contain chemical elements heavier than hydrogen, helium, lithium — and nickel.

It appears to be less enriched than Sol in elements heavier than hydrogen («metals») with about 72 - 89 percent of Sol's abundance of iron (Cayrel de Strobel et al, 1991, page 12).

The star may be as as enriched (102 percent) as Sol with elements heavier than hydrogen («metallicity»), based on its abundance of iron (Cayrel de Strobel et al, 1991, page 285).

The star appears to be have around 79 percent as enriched as Sol in elements heavier than hydrogen (Endl et al, 2008).

It is only 17 to 32 percent as enriched as Sol with elements heavier than hydrogen («metallicity»), based on its abundance of iron which includes Fe - 0.5 (James B. Kaler, 2002, pp. 21 - 22; and A. S. Gaudun, 1994).

Beta Virginis is nearly 1.4 times as enriched as Sol with elements heavier than hydrogen («metallicity») based on its abundance of iron and may be around 3.2 to 4.1 billion years old (North et al, 2009; Eggenberger and Carrier, 2006; and Thomas Gehren, 1978).

The star may be only 40 to 105 percent as enriched as Sol with elements heavier than hydrogen («metallicity»), based on its abundance of iron (Cayrel de Strobel et al, 1991, page 292).

Sensitive to estimate's of the star's abundance of «metals» (elements heavier than hydrogen), Star A appears to have 1.6 to 1.7 times Sol's mass (van Belle et al, 2007; Guenther et al, 2005; D.B. Guenther, 2004; and Carrier et al, 2004), about 2.7 times Sol's diameter (van Belle et al, 2007; Fracassini et al, 1994; and Johnson and Wright, 1983, page 679), and around 8.9 times Sol's bolometric luminosity (van Belle et al, 2007; and Thévenin et al, 2005).

It may be somewhat less enriched as Sol with elements heavier than hydrogen («metallicity») based on the ionization balance of iron and a comparison between observed and computed profiles for the extremely strong ionized calcium (Ruck and Smith, 1995)-- metallicity measurements based on iron alone range from 55 to 155 percent of Sol's (Cayrel de Strobel et al, 1991, page 26).

The star appears to be from 89 to 186 percent as enriched as Sol with elements heavier than hydrogen («metallicity»), based on its abundance of iron (Cayrel de Strobel et al, 1991, page 312).

It may only be about three to 10 percent as enriched as Sol in elements heavier than hydrogen (Cayrel de Strobel et al, 1991, page 20; and J. Tomkin, 1972).

Star Ba may be only 76 percent as enriched as Sol with elements heavier than hydrogen («metallicity»), based on its abundance of iron (Cayrel de Strobel et al, 1991, page 291).

Lacaille 9352 may have 50 to 58 of Sol's mass (Demory et al, 2009, Table 4; RECONS; and NASA Star and Exoplanet Database, interpolation table of Henry and McCarthy, 1993), less than half (43 to 46 percent) of its diameter (Demory et al, 2009, Table 4; and NASA Star and Exoplanet Database, derived from the power law formula of Kenneth R. Lang, 1980), 1.1 percent of its visual luminosity and 3.5 percent of its bolometric luminosity (NASA Star and Exoplanet Database, derived from the exponential formula of Kenneth R. Lang, 1980), and only about one tenth to 60 percent of Sol's abundance of elements heavier than hydrogen («metallicity»)(Demory et al, 2009, Table 4).

It appears to be more than twice (2.09 times) as enriched as Sol with elements heavier than hydrogen («metallicity»), based on its abundance of iron (exoplanets.org).

It is about 63 to 68 percent as enriched as Sol in elements heavier than hydrogen (metallicity), based on its abundance of iron (Cayrel de Strobel et al, 1991, page 5).

Given the low abundance of elements heavier than hydrogen, moreover, it is possible that the star is more likely to have gas giants in cold outer orbits.

H. Bond (STSci), R. Ciardullo (PSU), WFPC2, HST, NASA HD 147513 B is a young white dwarf (a remnant stellar core which enriched its binary companion, Star A) with elements heavier than hydrogen when it cast off its outer gas layers) like planetary nebula NGC 2440.

It appears to be «super metal - rich,» with around 1.4 to 2.0 times as enriched as Sol with elements heavier than hydrogen («metallicity») based on its abundance of iron (NASA Stars and Exoplanet Database; Feltzing and Gonzales, 2001; and Cayrel de Strobel et al, 2001).

According to the California Planet Research Team, Edasich may be slightly more (107 percent) enriched than Sol with elements heavier than hydrogen («metallicity») based on its abundance of iron exoplanets.org, although an earlier reference suggests that it is at least twice as enriched (Cayrel de Strobel et al, 1991, pp. 298 — and 294 to compare Epsilon Virginis with Sol).

The star may be 1.66 times as enriched as Sol with elements heavier than hydrogen («metallicity»), based on its abundance of iron (Klaus Fuhrmann, 1998).

HE 0107 - 5240 has the lowest, known abundance of elements heavier than hydrogen and helium of stars in the Milky Way Galaxy that have thus far been measured for «metallicity» (more).

Sirius A is rich in elements heavier than hydrogen («metals rich»), as it has about one to 7.4 times the iron abundance of Sol (Cayrel de Strobel et al, 1991, pages 285 - 286).

The star may only be around 66 to 141 percent as enriched as Sol with elements heavier than hydrogen («metallicity») based on its abundance of iron (NASA Stars and Exoplanet database; Valenti and Fischer, 2005; Takeda et al, 2002; and Cayrel de Strobel et al, 1991, page 299).

The star appears to be relatively enriched in elements heavier than hydrogen («metals») because it has 105 percent of Sol's abundance of iron (Cayrel de Strobel et al, 1991, page 282).

It may be at least as enriched as Sol in elements heavier than hydrogen («metals»), as it has between 54 and 214 percent of Sol's abundance of iron (Cayrel de Strobel et al, 1991, page 9).

It appears to be more enriched than Sol in elements heavier than hydrogen («metals») with between 1.05 to 2.29 times Sol's abundance of iron (Cayrel de Strobel et al, 1991, pages 294 - 295).

Extremely scarce in elements heavier than hydrogen and helium («metals»), HE 0107 - 5240 was found as part of a search for metal - poor halo stars in the Hamburg / ESO Survey, which gave it its «HE» designation in combination with its position (see: press releases from ESO and the University of Michigan; and Christlieb et al, 2002).

The data allowed them to confirm the mass of the planet as well as determine the approximate metallicity (a number of elements heavier than hydrogen and helium within a celestial body), and the primary composition of the planet's atmosphere.

By combining observations from NASA's Hubble and Spitzer space telescopes, researchers determined that, unlike Neptune and Uranus, the exoplanet has relatively low metallicity, an indication of the how rich the planet is in all elements heavier than hydrogen and helium.

The star may be only be 12 to 25 percent as enriched as Sol with elements heavier than hydrogen («metallicity») based on its abundance of iron (Cayrel de Strobel et al, 1991, page 302).

The star may be as much as 1.1 times as enriched as Sol with elements heavier than hydrogen («metallicity»), based on its abundance of iron (NASA Star and Exoplanet Database from Valenti and Fischer, 2005; and Cayrel de Strobel et al, 1991, page 295).

It appears to be 54 to 59 percent as enriched as Sol in elements heavier than hydrogen («metals») based on its abundance of iron (Howard et al, 2010, for HD 97658 on Table 1, page 3; Raghavan et al, 2010; and Valenti and Fischer, 2005).

It may be from 49 to 100 percent as enriched as Sol with elements heavier than hydrogen («metallicity»), based on its abundance of iron (Cayrel de Strobel et al, 1991, page 4).

It appears to be around 1.1 times as enriched as Sol with elements heavier than hydrogen («metallicity»), based on its abundance of iron (exoplanets.org).

Based on the abundance of iron to hydrogen, Star A appears to be 35 to 48 percent as enriched as Sol in «metals» — elements heavier than hydrogen and helium (Howard et al, 2014; Berger et al, 2006, Table 5).

It appears to be about 63 percent as enriched as Sol with elements heavier than hydrogen («metallicity»), based on its abundance of iron (Cayrel de Strobel et al, 1991, page 278).

u «For one, the galaxy seems to be significantly rich in «metals» — elements heavier than hydrogen and helium.

The star may only be around 0.71 to 1.2 times as enriched as Sol with elements heavier than hydrogen («metallicity») based on its abundance of iron (Yoichi Takeda, 2007; Luck and Heiter, 2006, page 3075, Table 3; Allende Prieto et al, 1999, page 30, Table 1 for HR 799; and Cayrel de Strobel et al, 1991, page 280).

Indeed, the AB system is significantly more enriched (1.7 to 1.8 times) in elements heavier than hydrogen («high metallicity») than our own Solar System (Chmielewski et al, 1992; Cayrel de Strobel et al, 1991, page 297; Furenlid and Meylan, 1984; and Flannery and Ayres, 1978).

Based on Altair's abundance of iron, the star appears to be twice as enriched as Sol with elements heavier than hydrogen («metallicity»), (Cayrel de Strobel et al, 1991, page 306).

The star may be more (132 percent) enriched than as Sol with elements heavier than hydrogen («metallicity»), based on its abundance of iron (see Ups And b at exoplanets.org).

This white dwarf's mass allows it to fuse elements slightly heavier than hydrogen, so it has a stable core of carbon and oxygen.

u A few stars might be Population III stars that became polluted with elements heavier than hydrogen and helium that fell into the star as dust.

The star may be about only 63 percent as enriched as Sol with elements heavier than hydrogen («metallicity») based on its abundance of iron (D. Gigas, 1986, but more recent findings on Vega's mild underabundance of metals can be found in Ilijic et al, 1998).