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. |
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Výsledky 1-5 z 21
Strana xiv
... wavelengths of the invisible infrared are longer than those of red light, while radio wavelengths are longer yet. Shorter than violet is the ultraviolet, which is followed by X-rays and by gamma rays, which have wavelengths billions of ...
... wavelengths of the invisible infrared are longer than those of red light, while radio wavelengths are longer yet. Shorter than violet is the ultraviolet, which is followed by X-rays and by gamma rays, which have wavelengths billions of ...
Strana xv
... wavelengths. Visual magnitude alone gives no idea of how much invisible infrared or ultraviolet radiation may be packed into starlight, nor does it give much information on red, blue, or violet. Fortunately, the stellar temperature ...
... wavelengths. Visual magnitude alone gives no idea of how much invisible infrared or ultraviolet radiation may be packed into starlight, nor does it give much information on red, blue, or violet. Fortunately, the stellar temperature ...
Strana xvi
... wavelength by a specific atom or ion. Stars are classified by the appearance of the spectrum. At the top is a class A ... wavelengths (that is, colors) that depend critically on how the electron cloud is structured. Change the number of ...
... wavelength by a specific atom or ion. Stars are classified by the appearance of the spectrum. At the top is a class A ... wavelengths (that is, colors) that depend critically on how the electron cloud is structured. Change the number of ...
Strana xxii
... wavelengths of light to appear shorter for an approaching body and longer for a receding one. The Doppler effect is detected in stars through slight wavelength shifts in the absorption lines. In the ideal case, a closely-spaced double ...
... wavelengths of light to appear shorter for an approaching body and longer for a receding one. The Doppler effect is detected in stars through slight wavelength shifts in the absorption lines. In the ideal case, a closely-spaced double ...
Strana xxiv
... lovely glowing, expanding shell misleadingly called a “planetary nebula.” Instead of absorption lines superimposed on a continuum, planetary nebulae produce the opposite—emission lines—at the same wavelengths at which the.
... lovely glowing, expanding shell misleadingly called a “planetary nebula.” Instead of absorption lines superimposed on a continuum, planetary nebulae produce the opposite—emission lines—at the same wavelengths at which the.
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