Пример использования стиля color.sty

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\pagecolor{black}	! сделать фон черным
\color{white}		! сделать основной (текущий) цвет белым

 цвет & пример \qquad \\
\multicolumn{2}{||c||}{Предопределенные цвета} \\
   black   & \qquad \textcolor{black}{Какой это цвет?} \\
   white   & \qquad \colorbox{gray}{\textcolor{white}{Какой это цвет?}} \\
   red     & \qquad \textcolor{red}{Какой это цвет?} \\
   green   & \qquad \textcolor{green}{Какой это цвет?} \\
   blue    & \qquad \textcolor{blue}{Какой это цвет?} \\
   cyan    & \qquad \textcolor{cyan}{Какой это цвет?} \\
   magenta & \qquad \textcolor{magenta}{Какой это цвет?} \\
   yellow  & \qquad \colorbox{gray}{\textcolor{yellow}{Какой это цвет?}} \\
\multicolumn{2}{||c||}{Цвета определенные пользователем} \\
   light-blue & \qquad \textcolor{light-blue}{Какой это цвет?} \\
   gray    & \qquad \textcolor{gray}{Какой это цвет?} \\
   mygray  & \qquad \textcolor{mygray}{Какой это цвет?} \\

Her X-1 is one the first X-ray binary pulsar discovered
by the eminent UHURU
satellite in 1972
\textcolor{red}{(Tananbaum et al. 1972, Giacconi et al. 1973)}
and since
then remains one of the most studied accretion-driven X-ray stellar
binaries. The pulsar is an accretion-powered magnetized rotating ($P=1.24 $s~)
neutron entering an eclipsing X-ray binary with a low-mass ($\sim 2 M_\odot$)
optical companion in a practically circular orbit with a period
of 1.7 d. The binary orbit inclination is $i=85-88^o$, the total
duration of the X-ray eclipse is around 20,000 s.
The optical counterpart, HZ Her, first
suggested by Liller (1972),  provides a classical example of
the reflection effect when the strong orbital modulation in optics is due to
a powerful illumination of the part of normal star atmosphere facing
X-ray source (Bahcall \& Bahcall 1972;
\colorbox{cyan}{Che\-re\-pash\-chuk et al.} 1972).
The amplitude of the reflection effect strongly increases
in ultraviolet and according to many optical UBV-photometrical data is
$\Delta m_V =1.45,
\Delta m_B =1.6, \Delta m_U=2.55 $.}

Already very first UHURU observations of Her X-1 revealed the presence of
a long-term 34.85-d cycle. Its properties have been so interesting
that practically all specialized X-ray satellites studied it
(among which
Copernicus ,
Ariel-5, Ariel-6 (\fcolorbox{red}{mygray}{Davison \& Fabian} 1974, 1977, Ricketts et al. 1982),
HEAO-1 (Gorecki et al. 1982, Soong et al. 1987),
Hakucho  and TENMA (Nagase et al. 1984, Ohashi et al. 1984),
EXOSAT (\"Ogelman \& Tr\"umper 1988),
Gin\-ga (Deeter et al. 1991),
Astron (Sheffer et al. 1992),
BATSE (Wilson et al. 1994),
and RXTE (see
RXTE data are shown in Fig. 1).

The gross shape of the X-ray light curve consists of a main-on X-ray state
with a mean duration of 7 orbital periods surrounded by two off-states each 4
orbital cycles in duration, and of a secondary short-on state of smaller
intensity with a typical duration of $\sim 5.5$ orbital cycles.