Results 191 to 200 of about 500,059 (233)

No-rank tensor decomposition via metric learning. [PDF]

Sci Rep
Bagherian M.
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Feedback mechanisms stopping the star formation in a pair of massive galaxies in the early Universe

Pérez-González P, D'Eugenio F, Pino BRD, Perna M, Uebler H, Maiolino R, Arribas S, Lamperti I, Bunker A, Carniani S, Charlot S, Willott C, Böker T, Parlanti E, Scholtz J, Venturi G, Barro G, Costantin L, Navarro IM, Dunlop J, Magee D, Cresci G.   +21 more
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Quasi-periodic X-ray eruptions years after a nearby tidal disruption event. [PDF]

Nature
Nicholl M, Pasham DR, Mummery A, Guolo M, Gendreau K, Dewangan GC, Ferrara EC, Remillard R, Bonnerot C, Chakraborty J, Hajela A, Dhillon VS, Gillan AF, Greenwood J, Huber ME, Janiuk A, Salvesen G, van Velzen S, Aamer A, Alexander KD, Angus CR, Arzoumanian Z, Auchettl K, Berger E, de Boer T, Cendes Y, Chambers KC, Chen TW, Chornock R, Fulton MD, Gao H, Gillanders JH, Gomez S, Gompertz BP, Fabian AC, Herman J, Ingram A, Kara E, Laskar T, Lawrence A, Lin CC, Lowe TB, Magnier EA, Margutti R, McGee SL, Minguez P, Moore T, Nathan E, Oates SR, Patra KC, Ramsden P, Ravi V, Ridley EJ, Sheng X, Smartt SJ, Smith KW, Srivastav S, Stein R, Stevance HF, Turner SGD, Wainscoat RJ, Weston J, Wevers T, Young DR.   +63 more
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Extreme energy in a relaxed galaxy group indicates the bursty nature of AGN feedback

Eckert D, Gastaldello F, Lovisari L, McGee S, Pasini T, Brienza M, Kolokythas K, O'Sullivan E, Simionescu A, Sun M, Bourne M, Chen Y, Cui W, Ettori S, Finoguenov A, Gozaliasl G, Kale R, Mernier F, Oppenheimer B, Schellenberger G, Seppi R, Tempel E.   +21 more
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Modes of the Dark Ages 21 cm field accessible to a lunar radio interferometer. [PDF]

Philos Trans A Math Phys Eng Sci
Bull P, Guandalin C, Addis C.
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Revisiting the Surface Brightness Profile of the Stellar Disk with the Statistical Mechanics of the Self-Gravitating System with the Central Body. [PDF]

Entropy (Basel)
Kang DB.
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Elliptical galaxies

, 2003
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ELLIPTICAL GALAXIES

, 2016
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Dynamics of Elliptical Galaxies

Science, 1993
Elliptical galaxies were once thought to be similar in their structure and dynamics to rotationally flattened bodies like stars. The discovery that elliptical galaxies rotate much more slowly than a fluid body with the same shape has led to a qualitative change in our understanding of the dynamics of these systems.
openaire   +2 more sources

Hydrodynamical models of elliptical galaxies

Celestial Mechanics, 1988
Hydrodynamical models of elliptical galaxies can be obtained by means of Jeans’equations (see for example Ortega and de Freitas Pacheco, 1986). Following this approach, we consider a mass distribution in steady state which approximates de Vaucouleurs’ r1/4 law, and assume the principal axes of the velocity distribution to be parallel to unitary vectors
E. Moreno, P. Pişmiş
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