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Her X-1 is one the first X-ray binary pulsar discovered
by the eminent UHURU
satellite in 1972 (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; 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 $.


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\caption{Рисунок высотой 1.5 см.}
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\caption{Рисунок в ширину колонки.}
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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 (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. The form of
the X-ray light curve is asymmetric: in the main-on state the X-ray
intensity rapidly increases during 1.5-2 orbital cycles, stays at maximum
over 2.5 cycles, and then decreases to a minimum in the successive 3 orbital
revolutions.

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