Astrophysics| Astrophysics |
In General > s.a. astronomy; fluid;
stars.
* 1997, Main issues:
GRB's, flares of TeV blazars, black holes and relativistic jets, uhe cosmic
rays, neutrino astronomy, extragalactic B fields,
and cosmological models.
* 2001, Big questions:
The NSF/DOE/NASA Committee on Physics and the Universe (CPU), chaired by M
Turner, proposed 11 big questions, (1) What
is dark matter? (2) What are the neutrino masses
and their consequences? (3) Are there additional spacetime
dimensions? (4) What is dark energy? (5) Are protons unstable? (6) How did
the universe begin? (7) Did Einstein
have the last word on gravity? (8) How do cosmic accelerators
work? (9) Are there new states of
matter at the highest densities and T's? (10) Is a new theory of matter
and light needed at the highest E's?
(11) How
were the elements from Fe to U made?
Astroparticle Physics / High-Energy Astrophysics > s.a. astrophysical
neutrinos; cosmic rays; particle physics.
@ Books, Reviews: Katz 87; Raffelt 96; Klapdor-Kleingrothaus & Zuber
97 [r PT(98)nov];
Jacob IJMPA(97);
Khlopov 99;
Bergström & Goobar 04 [r 1st
ed PT(00)mar];
Magnussen
hp/99-in;
Battiston ap/02-in
[from space]; Ellis ap/02-in;
Blandford ap/03-in;
Olinto ap/03-in;
Perkins 03; Sigl hp/04-in,
ap/06-in;
Gaisser
ap/05-in;
Olive ap/05-ln;
Stanev ap/05-in;
Westerhoff IJMPA(05);
Giovannelli NCB(05)
[open problems]; Kolb a0708 [essay];
Mavromatos a0708-in
[and collider hep]; Bettini IJMPA(07);
Berezinsky a0801-in;
Spiering a0804-AN
[status of field in Europe]; Cirkel-Bartelt LRR(08) [history].
@ Neutrinos: Balantekin & Haxton ap/99-in
[review]; Anchordoqui
et al PLB(05)
[as diagnostic].
@ Related topics: Chen AAPPS(03)ap,
Ng ap/03-in
[lab/accelerator experiments]; De Rújula ap/04-in
[unified "cannonball" model]; Schaffner-Bielich et al a0711 [role
of strangeness].
Star Formation and Evolution
* Formation: The main
model of star formation originated with the Jeans (1902) theory of the evolution
of density perturbations in a medium;
Below
a certain level, they propagate as sound waves; Above it they give rise
to
structure by gravitational instability [& Hoyle 53; Peebles & Dicke
68; Zel'dovich et al 67]; The exact evolution depends on what mechanisms are
available for energy loss; Not much is known in detail.
* Energy source: The sequence of nuclear reactions in stars was proposed
by Bethe (1938).
* Primordial stars: Population
III stars may have formed right after recombination (
5 ×
105 yr)
at masses of 10–2–10–3 MSun
(brown dwarves); This may account for a significant fraction of dark matter
and the high mass end, upon explosion, for the heavy elements found
in population
II stars.
* Problems with observation:
The neutrino problem and solar pulsations.
@ General references: Eddington; Smart 38 [classic]; Chandrasekhar 42, RMP(84);
Saslaw 85; Dejonghe
PRP(86);
Binney & Merrifield 98; Ray SA(00)aug [early life]; Gurzadyan ap/03-in
[dynamics and stability]; Smith 04;
Chrysostomou & Lucas CP(05);
McKee & Ostriker a0707 [formation].
@ Non-technical: Narlikar 85; Greene AS(01) [protostars]; Heavens AS(05)
[and galaxy history].
@ Primordial stars: & Rees 76, Silk 77, Muhanov & Ozernoy
95; Panagia ap/02-in
[first generations].
Compact Objects > s.a. black
hole phenomenology and
solutions; computational
physics; matter;
neutron stars.
* Accretion disks: They became important since the discovery of compact
binary X-ray sources.
* Eddington Limit: Ther maximum accretion rate, beyond which the pressure
from radiation emitted by the infalling matter would stop further accretion.
@
Accretion disks: Frank et al 85; Blaes SA(04)oct.
@ Instabilities: Chandrasekhar & Friedman PRL(71) [rotating star]; Bechhoefer & Chabrier AJP(93)
[in higher dimensions]; Villain ap/06-in.
@ Related topics: Blandford, Begelman & Rees SA(82)may [jets]; Shapiro & Teukolsky
83; Ziólkowski ap/05-in
[in Milky Way]; Lavagetto et al MNRAS(05)ap
[X-ray binaries and general relativity]; > s.a. Roche
Lobe.
Other Specific Topics > s.a. astronomical
objects [including
clusters]; early
universe; magnetism [plasmas].
* Buchdahl inequality:
For static spherically symmetric stars, under physically reasonable conditions,
the mass and radius satisfy 2M/R 
8/9;
A rhs of 1
would be the black hole limit.
@ Buchdahl inequality: Tsuchida et al PTP(98)gq [scalar-tensor
theory]; Andreasson gq/06 [spherical
static shells]; Heinzle a0708 [sharper inequality].
@ Radiative processes: Lightman & Rybicki 79.
@ Charge dynamics: Meier ApJ(04)ap/03 [highly relativistic].
References > s.a. history of
astronomy.
@ Reviews, books: Schatzman yr(70); Lang 80 [formulae]; Demianski 85;
Falcke & Biermann
ap/97-in;
Kitchin 98 [II]; Cox 00 [ref; r PT(00)oct];
Padmanabhan 00–01; Weinberg ap/01-in
[TX20]; Bhatia 02 [III]; Maoz 07.
@
Status: Trimble et al ap/06 [2005];
Trimble et al a0705 [2006].
@
Relativistic: van Putten 05 [gravitational radiation, black holes, GRB's];
Hoyng 06 [primer].
@ Stars in general relativity: Hartle ApJ(67);
Hartle ApJ(75);
Hartle & Friedman ApJ(75); Hartle & Munn ApJ(75);
Stergioulas LRR(98)ap-LRR(03),
Gergely et al gq/98-in
[rotating]; Nilsson & Uggla AP(01)gq/00,
AP(01)gq/00;
Passamonti et al PRD(05)
[oscillations].
@ Mathematical: Fridman & Polyachenko 84; Straumann 84.
@ Nuclear astrophysics: Burbidge et al RMP(57);
Arnould & Takahashi
RPP(99)ap/98;
Arnett ap/99-in
[explosive nucleosynthesis]; Lattimer & Prakash PRP(00)ap;
Brune ap/05-in
[rev]; Salpeter a0711 [early history].
@ Comments: Lopez-Corredoira ap/03 [research].
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sites – Acknowledgements
Send feedback and suggestions to bombelli at olemiss.edu – Modified
20 jun 2008