Problem of planetary systems existence. I. Methods and means of the search

Zakhozhay, V. A.

doi:10.18372/2411-6602.05.1034

Cited by 1 publication

(3 citation statements)

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“…Let us assume that the upper limit of the mass for population I stars is bounded by a high rate of stellar wind that exhausts rapidly the total mass of the star. In this case, the maximum stellar mass should obey the equality (10) For these stars, relationship (9) should be fulfilled, and their H times are determined using (5). When M = M maxI , substituting (5) and (9) into (10) yields (11) The solution to this equation yields a value of M maxI = 150.…”

Section: Maximum Masses Of Population I Starsmentioning

confidence: 99%

“…The relationship between the H time and the mass of zero age stars, i.e., the mass at which the hydrogen burning begins inside the star (further referred to as the mass), enables us to forecast which high luminosity stars could eventually host planetary systems (their lifetimes in the hydrogen burning stage should be longer than the time required for planets to form) [5]. The same relationship can be used to estimate the maximum masses of population I stars [4] since the stars with masses higher than 120 m ᭪ do not evolve through the giant stage [24].…”

Section: Introductionmentioning

confidence: 99%

“…logτ H -logM relationships(5) and(6)for the stars with solar (population I) and zero (population III) metal abundances.…”

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confidence: 99%

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Lifetimes of stars in the main sequence and the maximum mass of stars in the galactic disk

Zakhozhay

2013

Kinemat. Phys. Celest. Bodies

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Generalized and interconsistent approximation formulas are derived to describe the rela tionship between the hydrogen burning time and the zero age stellar mass for the mass and elemental composition ranges characteristic of stars that have been formed during the lifetime of the universe. The maximum masses of population I stars are estimated based on the known statistical relationships among stellar characteristics that agree with observational data. ZAKHOZHAYfor H times were given in [7] (for the solar elemental composition and masses of (0.2…100)m ᭪ , and higher than 100m ᭪ ) and in [3] (for masses of (1…100)m ᭪ , regardless of elemental composition).New numerical stellar models were obtained by Padova [10,15,16,[19][20][21] and GSEN [18,[43][44][45] teams in the 1990s. Based on these results, new "H time-mass" relationships were derived for the mass ranges (0.6…120)m ᭪ , (0.8…120)m ᭪ , and Z = 0.00007…0.03, 0.0004…0.05 in [41] and [12], respectively. The H times for masses of (0.6…120)m ᭪ and Z = 0.0004…0.05 are also tabulated in [40].The H time-mass relationships [12,40,41] calculated for the mass range (0.8…120)m ᭪ agree with each other within 10%, hindering the unambiguous choice of one of them. These results do not include H times for red dwarfs with masses lower than 0.6m ᭪ and metallicities of Z = 0 and Z = Z ᭪ . The cited papers provide expressions for the free terms a i (Z) that are functions of heavy nucleus abundances and cannot be used for our purposes. For Z =0, the values of coefficients in the free terms derived in [12] require a special anal ysis to ensure whether or not these correspond to the results of numerical modeling of zero metallicity stars [35,36,42,47], while those obtained in [41] approach infinity. Moreover, when the a i (Z) coefficients are used for masses of m > 100m ᭪ , the H times begin to increase, which contradicts the physical meaning.

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Section: Maximum Masses Of Population I Starsmentioning

confidence: 99%