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 53
Strana xi
... cores of stars provides the neccessary conditions. In the center of the Sun, the temperature is 16 million degrees Celsius, and the density is 150 times that of water. From the center out to about a quarter of the solar radius, protons ...
... cores of stars provides the neccessary conditions. In the center of the Sun, the temperature is 16 million degrees Celsius, and the density is 150 times that of water. From the center out to about a quarter of the solar radius, protons ...
Strana xiv
... cores, but are degraded by their passage through the stars' outer layers (in a process of continuous absorption and re-emission) into benign light. Though most stars are gaseous throughout, they can still be said to have “surfaces” at ...
... cores, but are degraded by their passage through the stars' outer layers (in a process of continuous absorption and re-emission) into benign light. Though most stars are gaseous throughout, they can still be said to have “surfaces” at ...
Strana xx
... cores. It is also a mass sequence that runs from around 100 solar masses at the top down to the minimum of 0.08 solar ... core, while the Sun has just 1 iron atom for every 32,000 of hydrogen. And iron atoms are populous compared with ...
... cores. It is also a mass sequence that runs from around 100 solar masses at the top down to the minimum of 0.08 solar ... core, while the Sun has just 1 iron atom for every 32,000 of hydrogen. And iron atoms are populous compared with ...
Strana xxi
... cores, which makes them very stable and long-lived. Stars of the middle main sequence turn into giants and then into white dwarfs, while the class O and hotter class B stars become supergiants and eventually explode. To this picture, we ...
... cores, which makes them very stable and long-lived. Stars of the middle main sequence turn into giants and then into white dwarfs, while the class O and hotter class B stars become supergiants and eventually explode. To this picture, we ...
Strana xxiii
... core, the structure of the entire star must respond and change. We use the laws of physics to calculate how the internal changes affect the star's outside appearance, namely its surface temperature and luminosity. When we do— behold!—we ...
... core, the structure of the entire star must respond and change. We use the laws of physics to calculate how the internal changes affect the star's outside appearance, namely its surface temperature and luminosity. When we do— behold!—we ...
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