Balmer series f() Blackbody absorption lines Balmer series Balmer continuum limit 365nm Schematic spectrum of a star,showing hydrogen Balmer lines and continuum.Absorption in Balmer continuum causes large deviation of stellar continuum from a blackbody spectrum and the U-B color index difference
Schematic spectrum of a star, showing hydrogen Balmer lines and continuum. Absorption in Balmer continuum causes large deviation of stellar continuum from a blackbody spectrum and the U-B color index difference
108 ^Balmer jump 盖 107 Pascthen jump 106 100 200 300 400 500 600 700 800 900 1000 Wavelength (nm) Model spectrum of the atmosphere of an A5-type star with T=8000 K
Model spectrum of the atmosphere of an A5-type star with T = 8000 K
486.1nm 364.6nm 2+ON 434.1nm +2- 空 410.2nm 群 罡 3300 3700 4100 4500 4900 λ(A) A digitally recorded spectrogram of a planetary nebula called IC 351
A digitally recorded spectrogram of a planetary nebula called IC 351. 486.1nm 434.1nm 410.2nm 364.6nm
恒星的光谱分类 ■恒星光谱：连续谱上叠加 700 nmHydrogen- 400nm 吸收线，少数恒星兼有发射 30,000K 线，或只有发射线 Helium 20,000K B 光谱分类：恒星连续谱的 Carbon- Helium 能量分布，谱线的数目和强 10,000K Calcium 度，特征谱线种类 7000K Sodium-Magnesium Oxygen Iron 光谱差异：不是因为化学 6000K 成分的不同；而是在不同温 Oxygen 4000K 度和压力下由恒星大气物质 的激发和电离状态的变化形 3000K 成的。 Titanium axide -Methyladine (CH)
恒星的光谱分类 n 恒星光谱：连续谱上叠加 吸收线﹐少数恒星兼有发射 线﹐或只有发射线 n 光谱分类：恒星连续谱的 能量分布﹐谱线的数目和强 度﹐特征谱线种类 n 光谱差异：不是因为化学 成分的不同；而是在不同温 度和压力下由恒星大气物质 的激发和电离状态的变化形 成的
Main Sequence Spectra L049L 19940H 05 HD46150 BO V HD46106 B5 V HD36936 y UMa 196V1 A3 V Coma T 183 HD27365 FO V Coma T 109 HD36300 F5 V 45Bo0 HD87431 GO V B Com HD36224 KO V y Ser oDra HD208812 F0 F2 F3F5 F6 F7 K5 V 61 Cyg A HD70896 M2V HD95735 ￥工 W56603 -H Il +H H pueq 189610 32 (A) (B)
F0 F2 F3 F5 F6 F7 F8