Astro Images with side notes
Open Earth Systems: An Earth Science Course For Maryland Teacher Professional Development EARTH HISTORY AND THE FOSSIL RECORD DAY 1 - Weds. July 9 AM Instruction:
Module : Activity 2: From After the ZAMS Module 8: Life on the Main Sequence Swinburne Online Education Exploring Stars and the Milky Way © Swinburne University.
From Pre-stellar Cores to Proto-stars: The Initial Conditions of Star Formation PHILIPPE ANDRE DEREK WARD-THOMPSON MARY BARSONY Reported by Fang Xiong,
Main criteria for classical PDRs are: - the sources cover a wide range of FUV field intensities and spectral shapes. - the sources have a well defined.
Evolution of isolated neutron stars: young coolers and old accretors Sergei Popov (SAI)
Solar vicinity, close-by young isolated NSs, and tests of cooling curves Sergei Popov (Sternberg Astronomical Institute) Co-authors: H.Grigorian, R. Turolla,
This set of slides This set of slides starts the topic of stellar evolution, overview, protostars, main sequence… Units covered: 59, 60, 61.
Spin evolution of NSs. 2 Hard life of neutron stars There are about 6 10 9 persons on Earth. How many do you know? There are about 1 10 9 NSs in the Galaxy.
Thermal evolution of neutron stars. Evolution of neutron stars. I.: rotation + magnetic field Ejector → Propeller → Accretor → Georotator See the book.
Close-by young isolated neutron stars (and black holes) Sergey Popov (Sternberg Astronomical Institute)
Spin evolution of NSs. 2 Evolution of neutron stars Thermal Magneto- rotational Observational appearence of a NS can depend on: Temperature Period Magnetic.
