From 64fdc7dc9fd8c68c18903595ca370874da8f18f9 Mon Sep 17 00:00:00 2001 From: vobolgus <130167730+vobolgus@users.noreply.github.com> Date: Sat, 31 Aug 2024 22:39:26 +0300 Subject: [PATCH] QSO added quasars to BH subsec --- data/spectrum-QSO.csv | 501 +++++++++++++++++++++++++++++++ sections/objects/black-hole.tex | 35 +++ sections/objects/degen-stars.tex | 6 +- sections/objects/nebulas.tex | 2 +- 4 files changed, 540 insertions(+), 4 deletions(-) create mode 100644 data/spectrum-QSO.csv diff --git a/data/spectrum-QSO.csv b/data/spectrum-QSO.csv new file mode 100644 index 0000000..04fb559 --- /dev/null +++ b/data/spectrum-QSO.csv @@ -0,0 +1,501 @@ +wavelength,flux +2960,0.057 +3238,0.064 +3312,0.071 +3351,0.08 +3378,0.072 +3400,0.067 +3419,0.066 +3436,0.07 +3452,0.069 +3467,0.064 +3482,0.066 +3484,0.094 +3484,0.063 +3488,0.068 +3491,0.076 +3495,0.069 +3497,0.057 +3503,0.07 +3511,0.046 +3512,0.067 +3518,0.071 +3521,0.07 +3525,0.036 +3531,0.063 +3538,0.033 +3542,0.05 +3552,0.043 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+7432,0.044 +7453,0.049 +7459,0.049 +7479,0.049 +7486,0.045 +7506,0.05 +7513,0.047 +7532,0.052 +7540,0.051 +7558,0.048 +7567,0.049 +7584,0.046 +7594,0.042 +7611,0.039 +7622,0.039 +7637,0.043 +7649,0.042 +7664,0.042 +7677,0.037 +7690,0.039 +7705,0.042 +7716,0.039 +7733,0.038 +7743,0.045 +7761,0.043 +7769,0.056 +7790,0.05 +7795,0.05 +7819,0.048 +7822,0.06 +7848,0.056 +7848,0.056 +7873,0.057 +7877,0.054 +7899,0.051 +7907,0.057 +7923,0.058 +7923,0.061 +7938,0.051 +7947,0.061 +7969,0.056 +7970,0.055 +7990,0.065 +8001,0.054 +8006,0.062 +8007,0.049 +8016,0.052 +8034,0.063 +8069,0.055 +8107,0.054 +8151,0.058 +8206,0.055 +8297,0.067 +8592,0.082 diff --git a/sections/objects/black-hole.tex b/sections/objects/black-hole.tex index 18243a4..2c3c52a 100644 --- a/sections/objects/black-hole.tex +++ b/sections/objects/black-hole.tex @@ -18,3 +18,38 @@ \subsection{Чёрные дыры} T = \frac{h c^3}{16 \pi^2 k G M}, \end{equation} где $k$ --- постоянная Больцмана. + +\term{Квазар}~— центральная область галактики с активным ядром, содержащая свермассивную черную дыру. Квазары представляют собой очень яркие и в то же время далекие и древние источники, поэтому ввиду их малого параллакса их зачастую используют для калибровки точных астрометрических инструментов. + +\begin{figure}[h!] + \centering + \tikzsetnextfilename{spectrum-QSO} + \begin{tikzpicture} + \footnotesize + \begin{axis} [ + height = 4cm, + width = \tw, + xlabel = {Длина волны $\lambda,~\mathring{\text{A}}$}, + ylabel style={ + text width=3cm, + align=center + }, + ylabel = Относительная\\интенсивность, + xmax = 7000, + xmin = 4000, +% xticklabels={4000, 5000, 6000, 7000, 8000, 9000}, +% xtick ={4000, 5000, 6000, 7000, 8000, 9000}, + ytick = {0, 1}, + ] + \addplot[smooth] table[x=wavelength, y=flux, col sep=comma]{data/spectrum-QSO.csv}; + \draw[thin] (axis cs:6500,0.3) -- (axis cs:6400,0.5) node[anchor=south] {$\text{H}_\alpha$}; + \draw[thin] (axis cs:4861,0.43) -- (axis cs:4800,0.6) node[anchor=south] {$\text{H}_\beta$}; + \draw[thin] (axis cs:4340,0.19) -- (axis cs:4340,0.4) node[anchor=south] {$\text{H}_\gamma$}; + + \draw[thin] (axis cs:5010,0.5) -- (axis cs:4980,0.8); + \draw[thin] (axis cs:4959,0.27) -- (axis cs:4980,0.8) node[anchor=south] {O\,III}; + \end{axis} + \end{tikzpicture} + \caption{Приведённый спектр квазара} + \label{pic:spectrum-QSO} +\end{figure} diff --git a/sections/objects/degen-stars.tex b/sections/objects/degen-stars.tex index 5935647..4547b0d 100644 --- a/sections/objects/degen-stars.tex +++ b/sections/objects/degen-stars.tex @@ -50,7 +50,7 @@ \subsection{Вырожденные звёзды} height=5cm ] \nextgroupplot[ - yticklabels={}, + yticklabels={0, 1}, xticklabels={}, xmin=3800, xmax=6200, ytick={0, 1}, @@ -59,7 +59,7 @@ \subsection{Вырожденные звёзды} \addplot[black, smooth] table[col sep=comma, x=wavelength, y=flux] {data/spectrum-DA.csv}; \nextgroupplot[ - yticklabels={}, + yticklabels={0, 1}, xmin=3800, xmax=6200, ytick={0, 1}, xtick={4000, 4500, 5000, 5500, 6000}, @@ -76,6 +76,6 @@ \subsection{Вырожденные звёзды} \label{pic:spectrum-wd} \end{figure} +\term{Нейтронная звезда}~--- сверхплотная звезда, образующаяся в результате взрыва Сверхновой. Вещество нейтронной звезды состоит в основном из нейтронов. Масса нейтронной звезды лежит в пределах от $0.1M_{\odot}$ до $2$\,--\,$2.8M_{\odot}$ (предел Оппенгеймера-Волкова). Размер данной звезды составляет лишь $10$\,--\,$20$~км, а плотность составляет $10^{16}$\,--\,$10^{18}$ $\text{кг}/\text{м}^3$. Дальнейшему гравитационному сжатию нейтронной звезды препятствует давление ядерной материи, возникающее за счёт взаимодействия нейтронов. Так как нейтронные звёзды образуются в результате коллапса массивных звёзд, то из-за сохранения момента импульса скорость их вращения может достигать $10^5$~км/с. При наличии сильного магнитного поля и быстром вращении нейтронная звзеда может наблюдаться с Земли как \term{пульсар}. -\term{Нейтронная звезда}~--- сверхплотная звезда, образующаяся в результате взрыва Сверхновой. Вещество нейтронной звезды состоит в основном из нейтронов. Масса нейтронной звезды лежит в пределах от $0.1M_{\odot}$ до $2$\,--\,$2.8M_{\odot}$ (предел Оппенгеймера-Волкова). Размер данной звезды составляет лишь $10$\,--\,$20$~км, а плотность составляет $10^{16}$\,--\,$10^{18}$ $\text{кг}/\text{м}^3$. Дальнейшему гравитационному сжатию нейтронной звезды препятствует давление ядерной материи, возникающее за счёт взаимодействия нейтронов. Так как нейтронные звёзды образуются в результате коллапса массивных звёзд, то из-за сохранения момента импульса скорость их вращения может достигать $10^5$~км/с. При наличии сильного магнитного поля и быстром вращении нейтронная звзеда может наблюдаться с Земли как \term{пульсар}. diff --git a/sections/objects/nebulas.tex b/sections/objects/nebulas.tex index 0c0954f..763feaa 100644 --- a/sections/objects/nebulas.tex +++ b/sections/objects/nebulas.tex @@ -48,7 +48,7 @@ \subsection{Планетарные туманности} % https://britastro.org/specdb/data_graph.php?obs_id=86&obs_validated=1&obs_observer_id=DDB&r_c=1&f_c=0&o_comment=&plot=Plot % https://britastro.org/specdb/data.php \label{pic:spectrum-m27} -\end{figure} +\end{figure} Спектр планетарной туманности состоит из эмиссионных линий тех элементов, из которых она состоит. Как было сказано выше, звезда сбрасывает оболочку уже после запуска синтеза тяжелых элементов из гелия. Одним из путей такого синтеза является CNO-цикл, на различных стадиях которого образуется, соответственно, углерод, азот и кислород. Ионизационное излучение которых можно наблюдать на спектре, например, \lookPicRef{pic:spectrum-m27}.