From e39701e7053f79daa423162b7aad5b42a8d13660 Mon Sep 17 00:00:00 2001
From: vobolgus <130167730+vobolgus@users.noreply.github.com>
Date: Tue, 23 Jul 2024 04:58:59 +0300
Subject: [PATCH] White dwarf sec

degen-stars section significantly expanded
---
 data/spectrum-DA.csv                | 501 ++++++++++++++++++++++++++++
 data/spectrum-DB.csv                | 501 ++++++++++++++++++++++++++++
 sections/objects/degen-stars.tex    | 107 ++++--
 sections/objects/variable-stars.tex |  34 +-
 style/astro-notebook.plot.sty       |   1 +
 5 files changed, 1114 insertions(+), 30 deletions(-)
 create mode 100644 data/spectrum-DA.csv
 create mode 100644 data/spectrum-DB.csv

diff --git a/data/spectrum-DA.csv b/data/spectrum-DA.csv
new file mode 100644
index 0000000..008b3e6
--- /dev/null
+++ b/data/spectrum-DA.csv
@@ -0,0 +1,501 @@
+wavelength,flux
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diff --git a/data/spectrum-DB.csv b/data/spectrum-DB.csv
new file mode 100644
index 0000000..41c3f2b
--- /dev/null
+++ b/data/spectrum-DB.csv
@@ -0,0 +1,501 @@
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diff --git a/sections/objects/degen-stars.tex b/sections/objects/degen-stars.tex
index e1dd696..02db181 100644
--- a/sections/objects/degen-stars.tex
+++ b/sections/objects/degen-stars.tex
@@ -1,35 +1,86 @@
 \subsection{Вырожденные звёзды}
 \term{Вырожденные звезды}~--- звезды, в которых силам гравитации противостоят силы давление вырожденного газа. К таким относятся \imp{белые карлики} и \imp{нейтронные звезды}.
 
-\begin{figure}[!h]
+\begin{wrapfigure}[16]{r}{0.4\tw}
     \centering
-    \begin{minipage}[c]{0.49\tw}
-        \tikzsetnextfilename{light-curve-b-lyr}
-        \begin{tikzpicture}
-            \begin{axis}[
-                height    =    4.5cm,
-                width    =    \tw,
-                xlabel    =    {Фаза},
-                ylabel    =    {Блеск $m$, $~^m$},
-                ymax    =    .7,
-                ymin    =    -.1,
-                y dir    =    reverse,
-                xmax    =    1,
-                xmin    =    .0
-                ]
-                \addplot[smooth] table[x=t, y=m, col sep = comma]{data/light-curve-B-Lyr.csv};
-            \end{axis}
-        \end{tikzpicture}
-    \end{minipage}
-    \hfill
-    \begin{minipage}[c]{0.49\tw}
-        \centering
-        \includegraphics[width = .9\tw]{b-lyr}
-    \end{minipage}
-    \caption{Кривая блеска переменной типа $\beta$\,Lyr}
-    \label{pic:b-lyr}
-    \vspace{-.8pc}
+    \vspace{-0.7pc}
+    \tikzsetnextfilename{mass-radius-wd}
+    \begin{tikzpicture}
+        \begin{axis}[
+            width    =    4cm,
+            height    =    6cm,
+            xmax     =    0.8,
+            xmin    =    -0.6,
+            ymax    =    -1.5,
+            ymin     =     -3.5,
+            ylabel    =    {$\log\frac{R}{R_{\astrosun}}$},
+            xlabel     =     {$\log\frac{M}{M_{\astrosun}}$}
+        ]
+            \addplot [domain=-0.6:0.146, samples = 100, black, smooth]{
+            ln(
+                (
+                    (1.4 / (10^x))^0.66 
+                    - 
+                    ((10^x) / 1.4)^0.66
+                )^0.5 
+                / 93.5
+            ) / ln(10)};
+        \end{axis}
+    \end{tikzpicture}
+    \caption{Зависимость масса-радиус для белых карликов}
+    \label{pic:mass-radius-wd}
+\end{wrapfigure}
+
+\term{Белые карлики}~--- проэволюционировавшие звёзды лишённые собственных источников термоядерной энергии и светящие за счёт остывания. Масса белого карлика находится в диапазоне от $0.6M_{\odot}$ до $1.44 M_{\odot}$. Верхняя границы массы белого карлика называется пределом Чандрасекара, звезда с массой больше данного предела не может существовать как белый карлик. Радиус белых карликов примерно в $10^2$ раз меньше солнечного, т.е. можно считать, что $R_\text{БК} \simeq R_\oplus$. Плотность белых карликов лежит в диапазоне $10^7$\,--\,$10^{10}$~$\text{кг}/\text{м}^3$. Зависимость масса-радиус для белых карликов имеет сложную форму \lookPicRef{pic:mass-radius-wd}. Вертикальная асимптота на графике соотвтетствует пределу Чандрасекара. 
+
+Спектры белых карликов отличаются от спектров невырожденных звёзд. Главной особенностью являются \imp{широкие линии поглощения}, также примечательно малое присутствие или вовсе отсутсвие слабых линий в спектре. Белые карлики принято выделять в отдельный спектральный класс D, а подклассов выделяют по принципу присутствия тех или иных спектральных линий в спектре. Основные подклассы:
+\begin{itemize}
+	\item \term{DA} — водородные белые карлики, составляют около 80\% от популяции белых карликов;
+	\item \term{DB} — гелиевые белые карлики, составляют около 20\% от популяции белых карликов.
+\end{itemize}
+Остальные подклассы представляются немногочисленными. Соотношение 80:20 между подклассами DA и DB объясняется эволюцией: на последних стадиях жизни у пульсирующий красных гигантов уже присутствует вырожденное ядро окруженное водородным слоевым источником. Вследствие накопления гелия в ядре периодически происходит \imp{гелиевая вспышка} — вырождение внешних гелиевых слоёв ядра и резкое ускорение реакций. Однако после выгорания накопленного гелия происходит очередной поджог водородного слоевого источника. Красный гигант может сбросить оболочку в любой стадии, при сбросе в период гелиевой вспышки образуется гелиевый белый карлик класса DB, а если сброс произошел в период горения водородного слоевого источника — обнажится водородный белый карлик класса DA. Длительность гелиевой вспышки составляет около 20\% от длительности цикла пульсации, что и объясняет соотношение водородных и гелиевых карликов. На \picRef{pic:mass-radius-wd} приведены типовые спектры белых карликов класса DA и класса DB.
+
+
+\begin{figure}[h!]
+    \centering
+    \tikzsetnextfilename{spectrum-wd}
+    \begin{tikzpicture}
+        \begin{groupplot}[
+            group style={
+            	group name=wdplot,
+                group size=1 by 2,
+                vertical sep=0.5cm
+            },
+            width=\tw,
+            height=5cm
+            ]
+            \nextgroupplot[
+                yticklabels={},
+                xticklabels={},
+                xmin=3800, xmax=6200,
+                ytick={0, 1},
+                xtick={4000, 4500, 5000, 5500, 6000},
+            ]
+            \addplot[black, smooth] table[col sep=comma, x=wavelength, y=flux] {data/spectrum-DA.csv};
+            
+            \nextgroupplot[
+                yticklabels={},
+                xmin=3800, xmax=6200,
+                ytick={0, 1},
+                xtick={4000, 4500, 5000, 5500, 6000},
+                xlabel={Длина волны $\lambda,~\,\mathring{\text{A}}$}
+            ]
+            \addplot[black, smooth] table[col sep=comma, x=wavelength, y=flux] {data/spectrum-DB.csv};
+        \end{groupplot}
+        \path (wdplot c1r1.outer north west)
+          -- node[anchor=south,rotate=90] {\textsf{Относительная интенсивность}}
+          (wdplot c1r2.outer south west)
+    	;
+    \end{tikzpicture}
+    \caption{Спектр водородного и гелиевого белых карликов}
+    \label{pic:spectrum-wd}
 \end{figure}
-\term{Белые карлики}~--- проэволюционировавшие звёзды лишённые собственных источников термоядерной энергии и светящие за счёт остывания. Масса белого карлика находится в диапазоне от $0.6M_{\odot}$ до $1.44 M_{\odot}$. Верхняя границы массы белого карлика называется пределом Чандрасекара, звезда с массой больше данного предела не может существовать как белый карлик. Радиус белых карликов примерно в $10^2$ раз меньше солнечного, т.е. можно считать, что $R_\text{БК} \simeq R_\oplus$. Плотность белых карликов лежит в диапазоне $10^7$\,--\,$10^{10}$~$\text{кг}/\text{м}^3$.
+
+
 
 \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/variable-stars.tex b/sections/objects/variable-stars.tex
index ee9e498..420c5bc 100644
--- a/sections/objects/variable-stars.tex
+++ b/sections/objects/variable-stars.tex
@@ -60,7 +60,7 @@ \subsection{Переменные звёзды}
 
 \term{Затменно-переменные} звёзды --- системы из двух звёзд, суммарный блеск которых периодически изменяется с течением времени. Причиной изменения блеска могут быть затмения звёзд друг другом, или изменение их формы взаимной гравитацией в тесных системах. На \picRef{pic:w-uma}\,--\,\ref{pic:b-lyr}  представлены кривые блеска затменно-переменных звёзд трёх основных типов.
 
-\begin{figure}[!h]
+\begin{figure}[h!]
     \centering
     \begin{minipage}[c]{0.49\tw}
         \tikzsetnextfilename{light-curve-w-uma}
@@ -90,7 +90,7 @@ \subsection{Переменные звёзды}
     \label{pic:w-uma}
 \end{figure}
 
-\begin{figure}[!h]
+\begin{figure}[h!]
     \centering
     \begin{minipage}[c]{0.49\tw}
         \tikzsetnextfilename{light-curve-b-per}
@@ -117,3 +117,33 @@ \subsection{Переменные звёзды}
     \end{minipage}
     \caption{Кривая блеска переменной типа $\beta$\,Per}
 \end{figure}
+
+\begin{figure}[h!]
+    \centering
+    \begin{minipage}[c]{0.49\tw}
+        \tikzsetnextfilename{light-curve-b-lyr}
+        \begin{tikzpicture}
+            \begin{axis}[
+                height    =    4.5cm,
+                width    =    \tw,
+                xlabel    =    {Фаза},
+                ylabel    =    {Блеск $m$, $~^m$},
+                ymax    =    .7,
+                ymin    =    -.1,
+                y dir    =    reverse,
+                xmax    =    1,
+                xmin    =    .0
+                ]
+                \addplot[smooth] table[x=t, y=m, col sep = comma]{data/light-curve-B-Lyr.csv};
+            \end{axis}
+        \end{tikzpicture}
+    \end{minipage}
+    \hfill
+    \begin{minipage}[c]{0.49\tw}
+        \centering
+        \includegraphics[width = .9\tw]{b-lyr}
+    \end{minipage}
+    \caption{Кривая блеска переменной типа $\beta$\,Lyr}
+    \label{pic:b-lyr}
+    \vspace{-.8pc}
+\end{figure}
diff --git a/style/astro-notebook.plot.sty b/style/astro-notebook.plot.sty
index f2b7e7e..594f38c 100644
--- a/style/astro-notebook.plot.sty
+++ b/style/astro-notebook.plot.sty
@@ -1,6 +1,7 @@
 \RequirePackage{pgfplots}
 \pgfplotsset{compat = 1.3}
 \usepgfplotslibrary{patchplots}
+\usepgfplotslibrary{groupplots}
 %\RequirePackage{patchplots}
 \pgfplotsset{
     width	=	14	cm,