搜索结果: 1-15 共查到“天体物理学 Method R”相关记录19条 . 查询时间(0.125 秒)
A method is presented here for investigating variations in the upper end of the stellar Initial Mass Function (IMF) by probing the production rate of ionizing photons in unresolved, compact star clust...
An iterative method in a probabilistic approach to the spectral inverse problem: Differential emission measure from line spectra and broadband data
the spectral inverse problem Differential emission measure
2011/1/11
Inverse problems are of great importance in astrophysics for deriving information about the physical characteristics of hot optically thin plasma sources from their EUV and X-ray spectra. We describe ...
Mass Transfer in Binary Stars using SPH. I. Numerical Method
galaxies active - line formation - radiation mechanism general - scattering - X-rays general
2010/11/12
We present new results from Monte Carlo calculations of the flux and equivalent width
(EW) of the Ni K fluorescent emission line in the toroidal X-ray reprocessor model of
Murphy & Yaqoob (2009, MN...
Classical Cepheids: Yet another version of the Baade-Becker-Wesselink method
Cepheids luminosities radii color excess
2010/11/16
We propose a new version of the Baade–Becker–Wesselink technique, which allows one to independently determine the colour excess and the intrinsic colour of a radially pulsating star, in addition to it...
Accurate Modeling of Weak Lensing with the sGL Method
Accurate Modeling of Weak sGL Method
2010/11/10
We revise and extend the stochastic approach to cumulative weak lensing (hereafter the sGL
method) rst introduced in Ref. [1]. Here we include a realistic halo mass function and density pro les to m...
The Cool-Core Bias in X-ray Galaxy Cluster Samples I: Method And Application To HIFLUGCS
Galaxies clusters general - X-rays galaxies clusters - Galaxies clusters intracluster medium
2010/11/16
Aims. When selecting ux-limited cluster samples, the detection eciency of X-ray instruments is not the same for centrally-peaked and at objects, which introduces a bias in ux-limited cluster samples...
A method to determine distances to molecular clouds using near-IR photometry
ISM dust extinction – ISM clouds – Stars distances – ISM individual objects L1517 –ISM Chamaeleon I –ISM
2010/11/15
Aims. To develop a method to determine distances to molecular clouds using JHK near-infrared photometry.Methods. The method is based on a technique that aids spectral classification of stars lying tow...
The Laboratory Complex for the Calibration of Photometers Using the Optical Method for Determination of the Water Vapor Content in the Earth Atmosphere
Instrumentation and Methods for Astrophysics (astro-ph.IM)
2011/1/7
We describe the laboratory complex for the calibration of photometers that are used in weather service to measure the water vapor content in the Earth atmosphere.
A New Method to Identify Nearby, Young, Low-mass Stars
Solar and Stellar Astrophysics (astro-ph.SR)
2010/12/29
We describe a new method to identify young, late-type stars within ~150 pc of the Earth that employs visual or near-infrared data and the GALEX GR4/5 database. For spectral types later than K5, we dem...
A New Method for Determining Geometry of Planetary Images
Instrumentation and Methods for Astrophysics (astro-ph.IM)
2010/12/27
This paper presents a novel semi-automatic image processing technique to estimate accurately, and objectively, the disc parameters of a planetary body on an astronomical image.
A new multi-dimensional general relativistic neutrino hydrodynamics code for core-collapse supernovae. I. Method and code tests in spherical symmetry
general relativistic core-collapse supernovae neutrino hydrodynamics code
2010/3/19
We present a new general relativistic (GR) code for hydrodynamic supernova simulations with neutrino transport in spherical and azimuthal symmetry (1D/2D). The code is a combination of the CoCoNuT hyd...
A Method for Judging Decay or Growth of the Magnetic Field of Pulsar
Pulsar—decay or growth of magnetic field—method of judgement
2010/9/15
This paper provides a method for judging growth or decay of the magnetic field of pulsar by using pulse period P, or frequency ν, and its first and second derivatives P˙, P¨ or ν˙, ν¨. The author uses...
Analysis of chromatic effects in the shift-and-add method
shift-and-add method chromatic effects
2009/7/10
Analysis of chromatic effects in the shift-and-add method。
SPH with radiative transfer：method and applications。
Seeing Measurements at San Pedro Mártir Observatory using the DIMM Method
San Pedro Mártir Observatory DIMM Method
2009/6/16
Seeing Measurements at San Pedro Mártir Observatory using the DIMM Method。