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 37
Strana xiv
... cool stars are red and hot stars are blue, in keeping with the energies of spectral colors. To an astronomer, “color” is a handy reference to temperature. Colors actually seen by eye are subtle, and the cause of sometimes vociferous, if ...
... cool stars are red and hot stars are blue, in keeping with the energies of spectral colors. To an astronomer, “color” is a handy reference to temperature. Colors actually seen by eye are subtle, and the cause of sometimes vociferous, if ...
Strana xv
... cool to fuse much of anything. However, to understand stars, we need total power, not just that seen at visual wavelengths. Visual magnitude alone gives no idea of how much invisible infrared or ultraviolet radiation may be packed into ...
... cool to fuse much of anything. However, to understand stars, we need total power, not just that seen at visual wavelengths. Visual magnitude alone gives no idea of how much invisible infrared or ultraviolet radiation may be packed into ...
Strana xvii
... cool, the spectral sequence must also correlate with temperature. The sequence stretches from around 50,000 K at class O, through 5800 K at class G (our Sun), to 2000 K at class M. The spectral sequence is not a chemical sequence, as it ...
... cool, the spectral sequence must also correlate with temperature. The sequence stretches from around 50,000 K at class O, through 5800 K at class G (our Sun), to 2000 K at class M. The spectral sequence is not a chemical sequence, as it ...
Strana xviii
... cool end and merging with F0, which runs to F9, and so on. On this finer scale, the Sun is a G2 star. Luminosity Class Temperature and its related spectral class by themselves are insufficient to describe the observed array of stars ...
... cool end and merging with F0, which runs to F9, and so on. On this finer scale, the Sun is a G2 star. Luminosity Class Temperature and its related spectral class by themselves are insufficient to describe the observed array of stars ...
Strana xix
... cool stars must be large in radius. An extreme M giant can have a total, or bolometric, luminosity 20 magnitudes (100 million times) greater than an M dwarf. At their biggest, they can have diameters over 100 times that of the Sun, and ...
... cool stars must be large in radius. An extreme M giant can have a total, or bolometric, luminosity 20 magnitudes (100 million times) greater than an M dwarf. At their biggest, they can have diameters over 100 times that of the Sun, and ...
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