'Mass radius' diaporamas de présentation

Lecture1. Structure of Neutron Stars

Lecture1. Structure of Neutron Stars. Sergei Popov (SAI MSU). Artistic view. For NSs we can take T=0 and neglect the third equation. Hydrostatic equilibrium for a star. For a NS effects of GR are also important. M/R ~ 0.15 (M/M ? ) (R/10 km ) -1 J/M ~ 0.25 (1 ms/P) (M/M ? )(R/10km) 2.

717 views • 57 slides

Ya. B. Zeldovich All-Moscow Seminar of Astrophysicists

Ya. B. Zeldovich All-Moscow Seminar of Astrophysicists. Plamen Fiziev LTF JINR Dubna. Models of Neutron Stars without Functional Relation between the Radius and Mass 16 December 201 Moscow. ?. Tolman-Opehgeimer-Volkov system. EOS.

533 views • 53 slides

200

Gravity. Falling Through the Earth!. Riding In an Elevator. Tides. Black Holes. 100. 100. 100. 100. 100. 200. 200. 200. 200. 200. 300. 300. 300. 300. 300. 400. 400. 400. 400. 400. 500. 500. 500. 5 0 0. 500.

621 views • 51 slides

Ya. B. Zeldovich All-Moscow Seminar of Astrophysicists

Ya. B. Zeldovich All-Moscow Seminar of Astrophysicists. Plamen Fiziev LTF JINR Dubna. Models of Neutron Stars without Functional Relation between the Radius and Mass 16 December 201 Moscow. ?. Tolman-Opehgeimer-Volkov system. EOS.

581 views • 43 slides

Termination of Stars

486 views • 37 slides

Constraining the Hadron-Quark Phase Transition Chemical Potential via Astronomical Observations

647 views • 32 slides

Planetary Sizes

Planetary Sizes. Dimitar Sasselov. Harvard-Smithsonian Center for Astrophysics. More diversity than expected ?. Some of the Hot Jupiters do not match well models based on Jupiter & Saturn:. Gaudi (2005) w Bodenheimer et al.(2003), Laughlin et al. (2005) models. Talk Plan.

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Timing of Transiting Planets Eric Agol, University of Washington

Timing of Transiting Planets Eric Agol, University of Washington. Three exoplanet problems:. Migration : Do Jupiters capture earths into (near) mean-motion resonance? Inclination : RV measures M * sin(I) I for non-transiting planets?

396 views • 27 slides

The structure and evolution of stars

The structure and evolution of stars. Lecture 12:White dwarfs, neutron stars and black holes. Learning Outcomes. The student will learn How to derive the equation of state of a degenerate gas How polytropic models can be applied to degenerate stars - white dwarfs

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Lecture (4)

Lecture (4). Previous lesson (1)Definition of moment of inertia. (2)Law of moment of inertia. (3)Math of moment of inertia. Lesson Decleared Polar moment of inertia and Radius of gyration. Learning outcomes

262 views • 9 slides