Below are the first 10 and last 10 pages of uncorrected machine-read text (when available) of this chapter, followed by the top 30 algorithmically extracted key phrases from the chapter as a whole.
Intended to provide our own search engines and external engines with highly rich, chapter-representative searchable text on the opening pages of each chapter.
Because it is UNCORRECTED material, please consider the following text as a useful but insufficient proxy for the authoritative book pages.
Do not use for reproduction, copying, pasting, or reading; exclusively for search engines.
OCR for page 65
Regular Variability of the Shape of the
Primary Minimum of the Orbital Light Curve
of SS 433 with the Phase of the Precessional Period
A.M. CHEREPASHCHUK AND S.~. YARLIKOV
Shternberg Astronomical Institute
The regular variations of the shape of the primary minimum of the
orbital 13.082-day light curio of SS 433 with the phase of the 1615~ay
precessional period have been discovered by analysis of the photomeuical
databank (1755 photometric V-observations during 1979 to 1988~. These
vanations with the characteristic period of about 26 days appeared near
the moment T3 of the maximum separation of the moving emission lines.
They are strongly connected with the phase ~ of the precessional 1615~ay
period (see Figure 1, where ^¢ = ~.023.
The variations within the period of approximately 26 days (see Figure
2) appeared and disappeared in asymmetry of the primary minimum of
orbital light curie and in changing position of the pnmaIy minimum for
A¢13 ~ ~ OP.1 (+ 1~.3) relatively the medium phase ~13 = 0 of orbital
13.082-day penod. In view of the fact of such variations the averaging of
observations ~ the Unwary minimum for the long interval of phases of the
precessional 162.5~ay period (~¢ > 0P.1) can lead to the false appearance
of "plate bottom" on the light curve in the puma minimum.
The regular vanability of the shape of the primary minimum of the
light curve of SS 433 discovered by us redects displacement with the 26-day
double orbital period of at least mo hot bright spots on the surface of
precessional accretional disk and their eclipse by a "normal" star. One of
"these spots can be connected with the ejection of the relativistic collimated
jet from the central part of the accretion disk; the second one perhaps is
caused by interaction of gas stream conlitlg from a "normal" star with an
external border of the precessional accretion disk
The precession of the accretion disk causes the change of the relative
position of hot spots. Consecutive eclipses of the disk and spots by the
"normal" star lead to the appearance and disappearance of asymmetry on
65
OCR for page 66
66
m
0.5
~ ,
AMERICAN AND SOVIET PERSPECTIVES
V ~ _ ~ I ~ I ~ ~ r · I' · t ~ ~ ~ ~ r r r
, ~ ~ r NO
: ~ yr=0.04
~ ~ y,= 0.98
I I ~I . ~. I . .
-
-
0 0.5 1 ~13
FIGURE 1 Optical orbital light Curares of SS433 as a function of the precessional period
fib.
the curve of the eclipse and to the characteristic features on it jUSt as it
takes place in cataclysmic variable stars.
Quantitative numerical interpretation of the discovered effect will be
completed in the future with the help of the light curve synthesis program
(Antolthina and CherepashchuL 1987. Astron. Zh 64: 562~.
OCR for page 67
HIGH-ENERGY ASTROPHYSICS
Min I
0.1
^~13
o
-0.1
0.6 0.8
67
(.) (a)
I)
my ()
(a) (by
, (V v162,5
it)
0.2 lo)
Min II
0.1 ~
0.6 0.8 O 0
-0.1
v13 ~ c,) t4 (-)
I'
t) 0) ()
ma_ a`
in, , ~ )
· (a) ()
' (I 1 v162,5
O.2 (,9 · 0.4
-
FIGURE 2 Varations of ~tb13 of the position of the pnmary minimum of optical light
curve of SS433 as a function of the phase of the precessional penod.
Representative terms from entire chapter:
primary minimum
