To construct two-dimension distribution of minor planets user should specify elements/ parameters/ function that will be plotted as abscissas and ordinates. In three-dimension case one should add to them the element plotted on Z axis. ... Though you may choose elements plotted along different axes at will, often there is good reason to plot such elements as a, n, or n" along X axis (two-dimension distributions) and to plot them along Y axis in three-dimension case. ...

... The Sun . ... The Corona . ... Solar Wind . 18H.Solar Wind obs. ... Field . ... The first indication that the sun might be emitting a "wind" came from comet tails , observed to point away from the Sun, whether the comet was approaching the Sun or whether it was moving away. ... The corona, like the Earth's atmosphere, is held down by the Sun's gravity. ... The particles at its "roots" stay with the Sun, but those in the high corona flow out with the solar wind, to the Earth's orbit and far beyond. ...

... Posts tagged ?light curve? ... Posted by hlee . ... Tags: book , Brieman , cigar , Clinton , data mining , Friedman , Hastie , KDD , light curve , machine learning , SCMA , shaking hands , SN , statistical learning , Supernova , Tibshirani . Category: Algorithms , Cross-Cultural , High-Energy , Jargon , Methods , Quotes , Stat , Uncertainty | Comment . ... Click for what was appeared in arXiv this week. ... Category: arXiv , Data Processing , gamma-ray , Objects , Spectral , Timing , X-ray | ...

... The Sun . ... The Corona . ... Solar Wind . 18H.Solar Wind obs. ... Field . ... The first indication that the sun might be emitting a "wind" came from comet tails , observed to point away from the Sun, whether the comet was approaching the Sun or whether it was moving away. ... The corona, like the Earth's atmosphere, is held down by the Sun's gravity. ... The particles at its "roots" stay with the Sun, but those in the high corona flow out with the solar wind, to the Earth's orbit and far beyond. ...

Chiaki Kobayashi, Ralph Sutherland How galaxies did form and evolution? - to answer this unsolved problem, we are simulating the formation and evolutionary history of galaxies in the Universe, including star formation, supernovae feedback, and chemical enrichment. Comparing the spacial distribution of elements within galaxies with observations, we will examine fundamental physical processes that drive galaxy formation. ... COALA : Universe Galaxy AGN Star Planet ...

... Armagh Observatory, College Hill, Armagh BT61 9DG, +44 (0)28 3752 2928 . ... Quasi-stationary electron distributions for the different values of the particle escape time. ... The electron-cyclotron maser instability is widespread in the Universe, producing, e.g., radio emission of the magnetized planets and cool substellar objects. ... The model used takes into account the radiation escape from the source region and the particle flow through this region. ...

... In brief: the frequency-dependent radiative transfer equation is solved for a dust under assumption of spherically-symmetric geometry for its distribution taking into account particle size distribution and quantum heating effects for the very small dust particles. ... Table: Model parameters for IRAS04296+3429. ... parameter . ... hot dust shell) . ... The best fit to the spectral energy distribution of IRAS04296 is shown by heavy solid line (see Table2 for details concerning parameters of the model...

Introduction This catalogue contains mainly the atomic data needed in the astrophysical investigations of low-density plasma. It is a revised and extended version of the "Catalogue of Atomic Data for the Rarefied Astrophysical Plasma" (Golovatyj et al. ... Low-density plasma. ... In the present study we represent only the atomic data for computation of sp ectra of low-density astrophysical plasma (most known kinds of it are gaseous nebulae), their thermal and ionization structure. ...

Next: Star Formation Rate and Up: No Title Previous: Calculation of Evolutionary Tracks . To start calculations, we choose the distributions of the initial binary parameters: the mass of the primary ZAMS component, , binary mass ratio, , orbital separation a . ... whereas the mass ratio distribution is not. ... The zero assumption often made is that the mass ratio distribution has a flat shape, that is binaries with a high mass ratio occur as frequently as those with equal masses. ...

... The polarimetry group at the Arcetri Observatory has been working for several years, mainly from the theoretical-interpretative side, on the polarization of the radiation emitted by objects of astrophysical interest. ... E. Landi Degl'Innocenti "The physics of polarization" in "Astrophysical Spectropolarimetry", J. Trujillo Bueno, F. Moreno Insertis, F. Sanchez (eds.), Cambridge University Press, 1. ... E. Landi Degl'Innocenti "The Zeeman effect: applications to solar physics" Astron. ...

... The distributions of orbits eccenttricities and of angular momenta for the halo stars and the old disk population are considered. The distributions have gaps separating the halo from the disk and dividing the halo population into three groups. ... Рассмотрены распределения звезд гало и старого населения диска по величине эксцентриситета орбит и угового момента. Распределения имеют провалы, отделяющие гало от диска и делящие населения гало на три группы. ...

Distribution of the analyzed SEPs with different >100 MeV proton fluxes ( J 100 ) at the microwave flux density plane ' S 9 vs. ... 1) General correspondence takes place between intensities of microwave bursts and proton fluxes - J 100 increases when S 9 and S 15 rise. ... 3) Powerful microwave bursts ( S 9 , S 15 >3000-10000 sfu ) with hard radio spectra ( S 9 < S 15 ) correspond to majority of powerful proton fluxes ( J 100 >10 pfu ). ...

... 2003 August 11 . Elements of the Swan Nebula . ... Explanation: In the depths of the dark clouds of dust and molecular gas known as M17 , stars continue to form. Also known as the Omega Nebula and Horseshoe Nebula, the darkness of M17's molecular clouds results from background starlight being absorbed by thick filaments of carbon-based smoke-sized dust . As bright massive stars form, they produce intense and energetic light that slowly boils away the dark shroud. ... About APOD | ...

Subject, Problems and Objects of Theoretical Astrophysics. ... Stellar Photospheres, Their Features. ... Physics of Continuous Radiation Absorption in Stellar Photospheres. ... Continuous Radiation Absorption in Stellar Photospheres of Various Spectral Classes. Solar Type Photospheres. ... Characterisics of Absorption Lines. ... Interstellar Absorption Lines, Their Features. ... Physical and Dynamic Features of Interstellar Medium, Which Follows from Observations of Interstellar Absorption Lines. ...

... For SIMS (Secondary Ion Mass Spectrometry) analysis, a solid surface is bombarded by primary ions of some keV energy. ... The subsequent mass analysis of the emitted ions provides detailed information on the elemental and molecular composition of the surface. ... Extremely short ion pulses with a duration below . ... By rastering a fine-focussed ion beam over the surface, like an electron beam in an electron microprobe, mass resolved secondary ion images (chemical maps) can be obtained...

... Does the time it takes different methods to create all the elements coincide with the universeт??s accepted age? ... Illinois Urbana-Champaign) Different kinds of stars create elements at different rates, all of which are consistent with the age of the universe. Get instant access to subscriber content on Astronomy.com! ... Registration is FREE and takes only a few seconds to complete. If you are already registered on Astronomy.com, please log in below. ...

... Using the central limit theorem, the total noise can be approximated by a Gaussian or normal distribution which has the frequency function : . ... where is the mean intensity of the source. ... In the statistical analysis of the probability distribution of data several estimators based on moments are used. ... For a normal distribution, these moments are and while for a Poisson distribution are and . Besides these moments other estimators are used to describe a distribution e.g. median and mode . ...

... Nizhnij Arkhyz, 2007 . ... Romanyuk I.I. Speech at the opening ceremony of the conference "Physics of magnetic stars" . ... Gnedin Yu.N. Magnetic fields of stars and fundamental particle physics . ... Landstreet J.D., Andretta V., Bagnulo S., Mason E., Silaj J., Wade G.A. The magnetic fields of peculiar A and B stars in open clusters . ... Wade G.A., Catala C., Alecian E., Folsom C., Bagnulo S., Bohm T., Bouret J.-C., Donati J.-F., Drouin D. , Landstreet J.D. Magnetic fields in Herbig Ae/Be stars . ...

... Research objects and scientific purposes . Space scientific program includes development and launch of two supersmall spacecrafts "Universitetskiy" and "Kompas-2" intended for monitoring of radiation conditions near the Earth. ... All the studies conducted in the near-Earth space are characterised by strong radiation fields. ... The circular polar orbits, which cover all the near-Earth space, are the most favorable for comprehensive studies of the radiation conditions near the Earth. ...

11 august 2014/Monday: Arriving, Registration . ... The variation of solar flare coronal X-ray source spatial properties. ... Melnikov V.F., Charikov Yu.E., Kudriavtsev I.V. Directivity of X-ray and gamma-ray emission from different parts of flaring magnetic loops. ... E., Melnikov V.F. Angular characteristics of polarization degree of hard X-ray emission from different parts of flaring magnetic loops. ... The thick target model and analytical calculations of the hard X-ray emission from solar flares. ...