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Bounds for joint spectral radii of a set of nonnegative matricesBounds for joint spectral radii of a set of nonnegative matrices are established by using

Bounds for joint spectral radii of a set of nonnegative matricesBounds for joint spectral radii of a set of nonnegative matrices are established by using

Joint bounds for the Perron roots of nonnegative matrices with applicationsGiven a finite set {Ax}x∈X of nonnegative matrices, we derive joint upper and lower bounds

Joint bounds for the Perron roots of nonnegative matrices with applicationsGiven a finite set {Ax}x∈X of nonnegative matrices, we derive joint upper and lower bounds

The neutron star in HESS? J1731 - 347: Central compact objects as laboratories to study the equation of state of superdense matter that is roughly two orders of magnitude lower than that of most of the radio and accreting pulsars. The thermal

The neutron star in HESS? J1731 - 347: Central compact objects as laboratories to study the equation of state of superdense matter that is roughly two orders of magnitude lower than that of most of the radio and accreting pulsars. The thermal

A neutron star stiff equation of state derived from cooling phases of the X-ray burster 4U 1724-307 by 15%) and the ratio of the stellar apparent radius to the distance. We then find a lower limit

A neutron star stiff equation of state derived from cooling phases of the X-ray burster 4U 1724-307 by 15%) and the ratio of the stellar apparent radius to the distance. We then find a lower limit

The effect of accretion on the measurement of neutron star mass and radius in the low-mass X-ray binary 4U 1608-52-state burst to put the lower limit on the NS radius R in 4U 1608-52 of 12 km (for masses 1.0-2.4M⊙). We

Influence of the Doppler effect on radiative transfer in a spherical plasma under macroscopic motion of substance

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