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262por Vockenhuber, C, Ouellet, C O, Buchmann, L, Caggiano, J A, Chen, A A, Crawford, H, D'Auria, J, Davids, B, Fogarty, L, Frekers, D, Hussein, A, Hutcheon, D A, Kutschera, W, Laird, A M, Lewis, R, O'Connor, E, Ottewell, D F, Paul, M, Pavan, M, Pearson, J, Ruiz, C, Ruprecht, G, Trinczek, M, Wales, B, Wallner, AEnlace del recurso
Publicado 2006
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268por Babak, Stanislav, Caprini, Chiara, Figueroa, Daniel G., Karnesis, Nikolaos, Marcoccia, Paolo, Nardini, Germano, Pieroni, Mauro, Ricciardone, Angelo, Sesana, Alberto, Torrado, Jesús“…We use the latest constraints on the population of stellar origin binary black holes (SOBBH) from LIGO/Virgo/KAGRA (LVK) observations, to estimate the stochastic gravitational wave background (SGWB) they generate in the frequency band of LISA.In order to account for the faint and distant binaries, which contribute the most to the SGWB, we extend the merger rate at high redshift assuming that it tracks the star formation rate.We adopt different methods to compute the SGWB signal: we perform an analytical evaluation, we use Monte Carlo sums over the SOBBH population realisations, and we account for the role of the detector by simulating LISA data and iteratively removing the resolvable signals until only the confusion noise is left.The last method allows the extraction of both the expected SGWB and the number of resolvable SOBBHs.Since the latter are few for signal-to-noise ratio thresholds larger than five, we confirm that the spectral shape of the SGWB in the LISA band agrees with the analytical prediction of a single power law.We infer the probability distribution of the SGWB amplitude from the LVK GWTC-3 posterior of the binary population model: at the reference frequency of 0.003 Hz it has an interquartile range of h$^{2}$Ω$_{GW}$(f = 3 × 10$^{-3}$ Hz) ∈ [5.65, 11.5] × 10$^{-13}$, in agreement with most previous estimates.We then perform a MC analysis to assess LISA's capability to detect and characterise this signal.Accounting for both the instrumental noise and the galactic binaries foreground, with four years of data, LISA will be able to detect the SOBBH SGWB with percent accuracy,narrowing down the uncertainty on the amplitude by one order of magnitude with respect to the range of possible amplitudes inferred from the population model. …”
Publicado 2023
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276por Scaringi, Simone, Maccarone, Thomas J., Körding, Elmar, Knigge, Christian, Vaughan, Simon, Marsh, Thomas R., Aranzana, Ester, Dhillon, Vikram S., Barros, Susana C. C.“…The central engines of disc-accreting stellar-mass black holes appear to be scaled down versions of the supermassive black holes that power active galactic nuclei. …”
Publicado 2015
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277por Kallinger, Thomas, Hekker, Saskia, García, Rafael A., Huber, Daniel, Matthews, Jaymie M.“…However, even with ultraprecise photometry from NASA’s Kepler mission, many stars are too faint for current methods or only moderate accuracy can be achieved in a limited range of stellar evolutionary stages. This means that many of the stars in the Kepler sample, including exoplanet hosts, are not sufficiently characterized to fully describe the sample and exoplanet properties. …”
Publicado 2016
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278por Welty, Francine K., Lewis, Sandra J., Friday, Karen E., Cain, Valerie A., Anzalone, Deborah A.“…This subgroup analysis of the Statin Therapies for Elevated Lipid Levels compared Across doses to Rosuvastatin (STELLAR) trial examines the effects of statin therapy in hypercholesterolemic women. …”
Publicado 2016
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279“…Integrating the advantages of INS (inertial navigation system) and the star sensor, the stellar-inertial navigation system has been used for a wide variety of applications. …”
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280por Ben-Aryeh, Y.“…The stability of low density stellar plasma is analyzed for a star with a spherical symmetry which is in equilibrium between the gravitational attractive forces and the repulsive pressure forces of an ideal electron gas where the analysis is developed by the use of Boltzmann statistics. …”
Publicado 2019
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