An Introduction to Modern Astrophysics An Introduction to Modern Astrophysics, Second Edition has been thoroughly revised to reflect the dramatic changes and advancements in astrophysics that have occurred over the past decade. The Second Edition of this market-leading book has been updated to include the latest results from relevant fields of astrophysics and advances in our theoretical understanding of astrophysical phenomena. The Tools of Astronomy: The Celestial Sphere, Celestial Mechanics, The Continuous Spectrum of Light, The Theory of Special Relativity, The Interaction of Light and Matter, Telescopes; The Nature of Stars: Binary Systems and Stellar Parameters, The Classification of Stellar Spectra, Stellar Atmospheres, The Interiors of Stars, The Sun, The Process of Star Formation, Post-Main-Sequence Stellar Evolution, Stellar Pulsation, Supernovae, The Degenerate Remnants of Stars, Black Holes, Close Binary Star Systems; Planetary Systems: Physical Processes in the Solar System, The Terrestrial Planets, The Jovian Worlds, Minor Bodies of the Solar System, The Formation of Planetary Systems; Galaxies and the Universe: The Milky Way Galaxy, The Nature of Galaxies, Galactic Evolution, The Structure of the Universe, Active Galaxies, Cosmology, The Early Universe; Astronomical and Physical Constants, Unit Conversions Between SI and cgs, Solar System Data, The Constellations, The Brightest Stars, The Nearest Stars, Stellar Data, The Messier Catalog, Constants, A Constants Module for Fortran 95 (Available as a C++ header file), Orbits, A Planetary Orbit Code (Available as Fortran 95 and C++ command line versions, and Windows GUI), TwoStars, A Binary Star Code (Generates synthetic light and radial velocity curves; available as Fortran 95 and C++ command line versions, and Windows GUI), StatStar, A Stellar Structure Code (Available as Fortran 95 and C++ command line versions, and Windows GUI), StatStar, Stellar Models, Galaxy, A Tidal Interaction Code (Available as Java), WMAP Data. For all readers interested in moden astrophysics. |
From inside the book
Results 1-3 of 78
Page 126
... produces dark absorption lines in the continuous spectrum . Absorption lines are produced when an electron makes a transition from a lower orbit to a higher orbit . If an incident photon in the continuous spectrum has exactly the right ...
... produces dark absorption lines in the continuous spectrum . Absorption lines are produced when an electron makes a transition from a lower orbit to a higher orbit . If an incident photon in the continuous spectrum has exactly the right ...
Page 362
... produced . In reality , the Fraunhofer lines are formed in the same layers where H produces the contin- uum . However , the darkest part of the line ( its center ) originates from regions higher in the photosphere , where the gas is ...
... produced . In reality , the Fraunhofer lines are formed in the same layers where H produces the contin- uum . However , the darkest part of the line ( its center ) originates from regions higher in the photosphere , where the gas is ...
Page 431
... produced at the same rate that free electrons and protons recombine to form neutral hydrogen atoms . When recombination occurs , the electron does not necessarily fall directly to the ground state but can cascade downward , producing a ...
... produced at the same rate that free electrons and protons recombine to form neutral hydrogen atoms . When recombination occurs , the electron does not necessarily fall directly to the ground state but can cascade downward , producing a ...
Other editions - View all
Common terms and phrases
absorption lines angle angular momentum approximately Assuming astronomers Astrophysics average axis Balmer binary blackbody radiation Boltzmann calculate center of mass cloud collapse constant convection core detector determined distance Earth eclipsing effective temperature electromagnetic emission emitted equilibrium estimate evolution Example FIGURE flux focal frame function Galaxy gravitational H-R diagram helium hydrogen atoms intensity ionization ions Kepler's kinetic energy light curve located luminosity magnetic field magnitude main sequence main-sequence stars measured molecular motion nebula neutrinos neutron star number density number of atoms object Observatory observed opacity optical depth orbital particles photons photosphere physical planet produced pulsar pulsation radial velocity radiation pressure radiative radio radius ratio relative relativistic result rotation Saha equation Section shown in Fig shows Sirius solar spectral lines spectral types spectrum speed star's stellar atmospheres Sun's supernova surface telescope vector wave wavelength white dwarf