The Hundred Greatest StarsSpringer Science & Business Media, 7. 5. 2006 - Počet stran: 211 I have always loved the stars. I watch them, photograph one. And you can hardly talk about Zubenelgenubi them, research them, write about them. Their wonder without bringing in Zubeneschamali, so they too are is that they are there not simply for scientists, but for treated within one story. The Sun is not included in the all of us, filling the night sky with their sparkling beauty. 100 list, but instead leads the pack as “Star Zero. ” There are as many different kinds as there are stars Before describing the glories of the 100 stars, an themselves, each an individual. The heavens give us introduction briefs the beginning stargazer on basic bright ones, dim ones, near ones, far ones, the aged, stellar properties and explains the astronomical the young, those that help tell our ancient stories, and terminology, without which we would be continuously those nearly invisible even with the greatest of our tongue-tied. A separate glossary provides a quick technologies. Taken together, they relate the tale of our reminder. Then we move on to the stars themselves. existence, of the birth, life, and death of the Sun on Each of my favorite stars is introduced by a short which we depend. |
Vyhledávání v knize
Výsledky 1-5 z 49
Strana xix
... supergiants. Within class M, these can be hundreds of times more luminous than run-of-the-mill giants. The largest would nearly span the orbit of Saturn, and in volume could hold over 1 billion suns. While supergiants span the whole ...
... supergiants. Within class M, these can be hundreds of times more luminous than run-of-the-mill giants. The largest would nearly span the orbit of Saturn, and in volume could hold over 1 billion suns. While supergiants span the whole ...
Strana xx
... supergiants (both of which actually merge with the dwarfs), and down at the lower left are the dim white dwarfs. Hypergiants lie at the top fringe of the supergiants. The main sequence is a zone of stable stars that fuse ordinary ...
... supergiants (both of which actually merge with the dwarfs), and down at the lower left are the dim white dwarfs. Hypergiants lie at the top fringe of the supergiants. The main sequence is a zone of stable stars that fuse ordinary ...
Strana xxi
... supergiants, we find different stellar sets in which hydrogen is nearly absent, leaving them very rich in helium and in carbon, nitrogen, and other elements. (These are not to be confused with the above “classical” carbon stars—they are ...
... supergiants, we find different stellar sets in which hydrogen is nearly absent, leaving them very rich in helium and in carbon, nitrogen, and other elements. (These are not to be confused with the above “classical” carbon stars—they are ...
Strana xxii
... supergiants, white dwarfs, and so on. Consequently, we can study the masses of the different varieties and correlate stellar mass with class and luminosity. The collection of studies shows that the main sequence is really a mass ...
... supergiants, white dwarfs, and so on. Consequently, we can study the masses of the different varieties and correlate stellar mass with class and luminosity. The collection of studies shows that the main sequence is really a mass ...
Strana xxiii
... supergiants to be nearly as massive as O dwarfs). Giants and supergiants are “too bright” for their masses (as compared to dwarfs), while white dwarfs are too dim. Observations of white dwarfs in double-star systems show them to have ...
... supergiants to be nearly as massive as O dwarfs). Giants and supergiants are “too bright” for their masses (as compared to dwarfs), while white dwarfs are too dim. Observations of white dwarfs in double-star systems show them to have ...
Obsah
2 | |
14 | 30 |
16 | 34 |
18 | 38 |
104 | 39 |
20 | 42 |
22 | 46 |
110 | 48 |
67 | 136 |
68 | 138 |
69 | 140 |
70 | 142 |
71 | 144 |
72 | 146 |
73 | 148 |
74 | 150 |
24 | 50 |
26 | 54 |
28 | 58 |
130 | 61 |
30 | 62 |
32 | 66 |
34 | 70 |
140 | 73 |
36 | 74 |
38 | 78 |
40 | 82 |
42 | 86 |
44 | 90 |
46 | 94 |
150 | 97 |
48 | 98 |
50 | 102 |
51 | 104 |
52 | 106 |
53 | 108 |
54 | 110 |
55 | 112 |
56 | 114 |
57 | 116 |
58 | 118 |
59 | 120 |
60 | 122 |
61 | 124 |
62 | 126 |
63 | 128 |
64 | 130 |
65 | 132 |
66 | 134 |
HZ 21 | 152 |
Mizar and Alcor Mu Cephei Mu Columbae MXB 1730335 | 153 |
76 | 154 |
200 | 155 |
77 | 156 |
78 | 158 |
79 | 160 |
80 | 162 |
81 | 164 |
82 | 166 |
83 | 168 |
84 | 170 |
85 | 172 |
86 | 174 |
87 | 176 |
88 | 178 |
89 | 180 |
90 | 182 |
91 | 184 |
92 | 186 |
93 | 188 |
94 | 190 |
95 | 192 |
96 | 194 |
97 | 196 |
98 | 198 |
99 | 200 |
100 | 202 |
STAR | 203 |
Acrux Adhara AG Draconis Albireo Algol Alpha Centauri Alphard Antares Arcturus Barnards Star Beta Canis Majoris Beta Cassiopeiae Beta Lyrae B... | 204 |
RS Ophiuchi SGR 1900+14 Sigma Octantis Sirius 16 Cygni 61 Cygni Spica SS Cygni SS 433 | 205 |
HD 93129A | 207 |
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Absolute visual magnitude absorptions accretion Alpha astronomers atoms Beta binary black hole bright brighter brightest brown dwarfs Capella carbon carbon stars Cassiopeiae celestial central stars Cephei cloud companion constellation cool core Cygni Cygnus Delta Delta Cephei disk distance double star dust Earth eclipse emissions energy Epsilon Eridani Eta Carinae fainter fusing fusion Galaxy Galaxy’s Gamma giant star gravity helium Hubble Space Telescope hydrogen infrared interstellar ionized J. B. Kaler kilometers per second light luminous Lyrae magnetic fields main sequence million Mira Mizar naked-eye neutron star nova Observatory Ophiuchi orbit Orionis pair percent period planetary nebula planets Polaris pole pulsar radiation radio radius Residence rotation second-ascent seconds of arc Sigma Octantis Significance Sirius solar luminosities solar masses spectral spectrum speed spin star’s stellar subgiant supergiant supernova surface surrounding Tauri temperature Thuban tion Tycho’s Ursa variable Vega visible wavelengths white dwarf wind X-ray