content stringlengths 34.5k 188k | data_id stringlengths 13 13 |
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label{eq:LnCdns}
\begin{aligned}
&{x\_{i,i+1}} - {r\_{i,i+1}}\geq 0 \\
&{v^{(t\_i-1)}\_{i}}{v^{(t\_i-1)}\_{i+1}}-4{P^{(t\_i+1)}\_{i,i+1}}{r\_{i,i+1}}{v^{(t\_i-1)}\_{i+1}}- \\
&\hspace\*{0.87in} 4{P^{(t\_i)}\_{i+1,i+2}}{r\_{i+1,i+2}}{v^{(t\_i-1)}\_{i}}\geq 0 \\
&{v^{(t\_i-1)}\_{i}} {v^{(t\_i-1)}\_{i+1}} - 4{P^{(t\... | arxiv_0186014 |
sustained anisotropy would change the orbital evolution of a planet within 100 au from its predicted isotropic adiabatic value.
In summary, given the mass values in Table [stelprop], the semimajor axis of an orbiting planet would likely increase by a factor of 4.4–5.6. For the lower mass stars usually considered in po... | arxiv_0186015 |
in 12CO. By assuming the LTE conditions, optically thin emission, a rotational temperature of 80 K, and an abundance ratio of [SiO]/[H2] = 10− 7, Zapata et al. (2006) estimated the total mass, momentum, and energy in those SiO outflows to be 1.155 M⊙, 57.85 M⊙kms− 1, and 3.03 ⋅ 1046 ergs. However, as suggested by the ... | arxiv_0186016 |
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