مصادر الصور

(1-1) A parsec.

(2-1) A dark globule (© European Southern Observatory/Science Photo Library).

(3-1) Luminosity of stars as a function of surface temperature.

(3-2) The planetary nebula Messier 57 (NASA and The Hubble Heritage Team (STScI/AURA)).

(3-3) The outer layers of the Sun.

(3-4) Magnetic field lines.

(3-5) Plasma draining down magnetic field lines.

(3-6) Magnetic field lines brought together.

(3-7) The globular cluster NGC 7006 (ESA/Hubble & NASA).

(3-8) Brightness versus colour for stars in a globular cluster (A. Sarajedini et al., “The ACS Survey of Galactic Globular Clusters. I. Overview and Clusters without Previous Hubble Space Telescope Photometry”, The Astronomical Journal, Volume 133, Issue 4, pp. 1658–1672 (2007), http://iopscience.iop.org/1538-3881/133/4/1658/, after W. E. Harris, AJ, 112, 1487 (1996). © AAS. Reproduced with permission).

(4-1) An accretion disc.

(4-2) Temperature versus radius in an accretion disc.

(4-3) The luminosity radiated by an accretion disc.

(4-4) The temperature of an accretion disc around a black hole of mass 10⁸ .

(4-5) The luminosity radiated outside radius (r) for a disc around a 10⁸ black hole.

(4-6) Gas is lifted off a disc by DQ Her (© Russell Kightley/Science Photo Library).

(4-7) Four snapshots of magnetic field lines in an accretion disc.

(4-8) The Herbig-Haro object HH30 (C. Burrows (STScI & ESA), the WFPC 2 Investigation Definition Team, and NASA).

(4-9) The geometry SS433.

(4-10) A radio image of the corkscrew jets of the binary star SS433 (K. M. Blundell & M. G. Bowler, using the U.S. National Radio Astronomy Observatory’s Very Large Array telescope; Astrophysical Journal 616, L159 (2004)).

(4-11) A radio image of the radio galaxy Cygnus A (Image courtesy of National Radio Astronomy Observatory/AUI).

(5-1) An orbital ellipse of eccentricity e = 0.5.

(5-2) The inclination angle between the invariable plane and the plane of the planet’s orbit.

(5-3) The positions of two planets on similar orbits shown at a hundred equally spaced times.

(5-4) A planet orbiting an (invisible) central star (F. Masset (UNAM)).

(6-1) Angular distribution of emission from jets.

(6-2) The geometry of superluminal expansion.

(6-3) The apparent velocity of a blob.

(6-4) Plasma coming fast from the left hitting slower-moving plasma on the right.

(6-5) Computer simulation of a jet-inflated cocoon (M. Krause, “Very Light Jets II: Bipolar large scale simulations in King atmospheres”, Astronomy & Astrophysics, 432, 45 (2005) reproduced with permission ©ESO).

(6-6) A lens and a gravitational lens.

(6-7) Weak lensing in the galaxy cluster Abell 2218 (W. Couch (University of New South Wales), R. Ellis (Cambridge University), and NASA/ESA).

(6-8) The micro-lensing event OGLE-2006-BLG-109 (Gaudi et al., “Discovery of a Jupiter/Saturn Analog with Gravitational Microlensing”, Science, 319, 927 (2008). © AAAS. Reproduced with permission via Copyright Clearance Center, Inc.).

(7-1) Galaxy luminosity function (D. H. Jones et al., “Near-infrared and optical luminosity functions from the 6dF Galaxy Survey”, MNRAS, 360, 25 (2006)).

(7-2) An image of our Galaxy (2MASS/J. Carpenter, T. H. Jarrett, & R. Hurt. Atlas image obtained as part of the Two Micron All Sky Survey (2MASS), a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the National Science Foundation).

(7-3) Cartoon of disc, bulge, and halo.

(7-4) Formation of a wake behind a massive body.

(7-5) Tides without a moon.

(7-6) A simulation of tidal tails forming (J. L. Sanders & J. Binney, “Stream-orbit misalignment-II. A new algorithm to constrain the Galactic potential”, MNRAS, 433, 1826 (2013)).

(7-7) Stars formed in the first gigayear (Recto-Blanco et al. (2014)).

(7-8) The Coma cluster ((a) NOAO/AURA/NSF TBC; (b) S. L. Snowden USRA, NASA/GSFC).

(7-9) A dwarf galaxy and cold, star forming gas (Geha et al., Astrophysical Journal, 653, 240 (2006), fig. 4).