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Artemisa Villalobos-Ramirez

Publications and source records attributed to Artemisa Villalobos-Ramirez.

2 recordsLinked to original sources

Dressed-state master equation for two strongly coupled two-level atoms with long-lived entanglement

We derive a dressed-state master equation in Lindblad form for two strongly coupled two-level atoms. The resulting decay dynamics are governed by Lindblad operators that couple different dressed states. We show that the eigenvalues and eigenvectors of the Liouvillian can be obtained in a compact form, since each off-diagonal element in the dressed-state basis constitutes an eigenvector. Depending on the interatomic distance and the atomic transition frequency, the decay exhibits two well-separated time scales. On short times, the system relaxes into a pair of states, one of which is a transient, maximally entangled state. On longer times, this intermediate entanglement irreversibly decays into a separable steady state. Our results demonstrate that the intrinsic decay mechanism can transiently generate maximal entanglement, an effect that is not captured without the dressed-state master-equation formalism.

quant-ph↗

A general relativistic estimation of the black hole mass-to-distance ratio at the core of TXS 2226-184

In this work we make use of a general relativistic method to estimate the mass-to-distance ratio M/D = 3.54^{+0.2}_{-0.2} X 10^4 M_{sun}/Mpc of the black hole hosted at the core of the active galactic nucleus of TXS 2226-184, along with its Right Ascension offset and the recession redshift (velocity) of the galaxy. Our statistical fit is based on the frequency shift of photons emitted by water masers and their orbital positions when circularly revolving around the black hole center within the accretion disk of the active galactic nucleus. By taking into account a previously reported distance to the galaxy, we compare the result of the black hole mass fit to an estimate based on a mass-luminosity correlation. We find that the black hole mass at the core of TXS 2226-184 obtained with the aid of the statistical fit using the general relativistic method, M = 3.67 ^{+0.2}_{-0.2} X 10^6 M_{sun}, is approximately 0.6 times the black hole mass, M_{BH} = 6.24^{+3.6}_{-2.3} X 10^6 M_{sun}, computed with the mass-luminosity correlation.

astro-ph.GA↗