Astronomy and astrophysics with

By S. Klein. 2008

586 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Computational Mechanics

View Paper: https://www.semanticscholar.org/paper/000f9e8b85021cd817fc0cd993f953d9067312c7

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In Astronomy and Astrophysics

In Computational Mechanics

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Curvature profiles as initial conditions for primordial black hole formation (2006, unknown): “−s”
LRS Bianchi type I models with anisotropic dark energy and constant deceleration parameter (2008, unknown): “48 67 v2 [ gr -q c] 1”
The origin of spin in binary black holes (2019, methodology): “The SFR formula we adopt is computed from UV and infrared surveys and is an updated version of Madau & Dickinson (2014) that better reproduces recent results at high redshifts 4 ≤ z ≤ 10 (Bowler et al. 2015; Finkelstein et al. 2015; Ishigaki et al. 2015; McLeod et al. 2015, 2016; Oesch et al. 2015).”
A Bayesian approach to strong lensing modelling of galaxy clusters (2007, background): “Many techniques have been proposed so far to find the roots of the lens equation (see e.g. Dominik 1995).”
Multifractal detrended fluctuation analysis of sunspot time series (2005, background): “(2011) E 09001 ournal of Statistical Mechanics:J Theory and Experiment”
COrE (Cosmic Origins Explorer) A White Paper (2011, background): “Mirrors: The PLANCK telescope has demonstrated that the technology needed already exists [289].”
Accretion-driven turbulence as universal process: galaxies, molecular clouds, and protostellar disks (2009, unknown): “The typical stellar velocity dispersion measured in nearby T Tauri associations or open star clusters is similar: ∼0.3 km s−1 for the Hyades (Madsen 2003), ∼0.5−0.6 km s−1 for Coma Berenices, Pleiades, and Praesepe (Madsen et al. 2002), and below ∼1 km s−1 for α Per (Makarov 2006), Lupus (Makarov 20”
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Reionization and Cosmology with 21-cm Fluctuations (2009, background): “However the distribution of fluctuation amplitudes becomes non-Gaussian as reionization progresses (Wyithe & Morales 2007, Harker et al. 2009), particularly on small scales when HII regions are formed (Furlanetto, Zaldarriaga & Hernquist 2004a, Bharadwaj & Ali 2005).”
BANYAN. XI. The BANYAN Σ Multivariate Bayesian Algorithm to Identify Members of Young Associations with 150 pc (2018, background): “In the literature, stars are typically considered bona fide members when they benefit from signs of youth and full kinematic measurements that allow them to be placed in XY ZUVW space (Malo et al. 2013; Gagné et al. 2014). The indicators of youth used in the literature depend on the spectral type of”
Galaxy formation theory (2010, background): “These scalings are consistent wi th a broad range of observations of star formation in di fferent galaxies. Similarly, Krumholz et al. (2009) find that the following exp ression encapsulates the complex physics of star formation:”