The high energy emissions from cataclysmic variables (interacting binary systems containing an accreting white dwarf) and the relationship of the high energy emission of these stars to their optical properties were investigated. The relationship of the cataclysmic binaries to the strong X-ray emitting binaries that contain a neutron star as the accreting star was examined. A soft X-ray survey of cataclysmic variable stars was carried out. Approximately 75% of all the sources observed were detected in short (2000 sec) observations. Relationships between the X-ray and optical luminosity and the dependence of this quantity on the subclass of the variable were investigated and constraints on the nature of these systems were provided

Lampton, M.

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https://ntrs.nasa.gov/search.jsp?R=19830010346 2020-03-21T05:41:40+00:00Z
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(NASA -C8-16978 0) TBE NAOTRE OF DVARF NOVAE 	 983-18617
AND SELA11C SZSTEPIS Final Technical Report
(California Oniv,) 7 p HC A02/NF 
AOCSCI. 031	 Unci$sG3/89 08701
FINAL TECHNICAL REPORT
NASA Grant NAGW-44
"The Nature of Dwarf Novae and Related Systems"
Dr. Michael Lampton, Principal Investigator
UNIVERSITY OF CALIFORNIA, BERKELEY
BEMELEY - DAVIS - IRVINE - LOS ANGELES - RIVERSIDE • SAN DIEGO - SA
(415) 642-1361
TWX: 11C SPACE BERK
(910) 366-'1945
Approved by:
IJA
Dr. 1ichae Lampt
January 27, 1983
Final Refit on NASA Grant NAGW-44
NASA grant NAGW-44 was awarded in order to further our understanding of
the high energy emissions from oataelysmio variables (interacting binary
systems containing an accreting white dwarf) and to study the relationship
of the high energy emission of these stars to their optical properties. A
subsidiary aim was to examine the relationship of the cataclysmic binaries
to the strong X-ray emitting binaries that contain a neutron star as
accreting star.
The research done under this grant has resulted in a number of
publications as listed at the end of the report. The following is a brief
summary.
A soft X-ray survey of cataclysmic variable stars has been carried out
using the Einstein observatory. Approximately 75% of all the sources
observed were detected in short (2000 sec) observations. Relationships
between the X-ray and optical luminosity and the dependence of this quantity
on the subclass of the variable have been investigated and have provided
constraints on the nature of these systems. The results have been reported
by Cordova, Mason and Nelson (1981), and Cordova and Mason (1981 and 1982).
A final paper which includes information on the variability of the sources
is almost complete (Cordova and Mason 1982).
Still on the subject of X-ray observations, HEAO-1 soft X-ray pointed
data on the cataclysmic variables U Gem and SS Cyg during outburst have been
.'
	
	
analysed. These two dwarf nova are, so far, the only members of their
subclass which have been found to show an intense ultra-soft X-ray emission
component during outburst.
	
In both cases the emission exhibits
quasi-periodic pulsations, with periods of order 25s and 9s for U Gem and
	PAGE 2	 -
33 Cyg respec-.ively. The observational properties of this emiselion have
been defined and mathematical medals of the potations constructed.
Optical observations have been conducted of cataclysmic variables and
related close binary X-ray sources. A previously uncatalogued dwarf nova,
	
E1551+718 9 has been identified with an X-ray source observed serendipitously 	 i
in the same field as another target and is reported by Mason et al (1982).
	A number of HEAD-1 soft X-ray sources have been surveyed with the Einstein 	
I
detectors in order,to reduce their positional uncertainties. Two of these
have been optically identified with Pew variables of the AM Her class (only
four of these were known previously). A paper discussing the
identification, optical spectrum and optical time variability of one of
these sources, E1405-451 9 has been submitted for publication (Mason et al
1982). A paper on the second, E1013-477,
 is in preparation. High time
resolution optical photometry of the X-ray pulsar 4U 1626-67 has revealed
the orbital period of the system to be 40 minutes. This is the shortest
orbital period known in this class of star (Middleditch et al 1981). An
optical burst, lasting -PO seconds, has been observed from the X-ray source
4U 1254-69 which was not previously known to be a burster (Mason et al.
1980). This is the first time that a burst source has been catalogued in
the optical region of the spectrum.
Ultraviolet, optical and infrared photometry and time resolved optical
spectroscopy has been obtained of the X-ray source 2A 1822 -371, which was
discovered to be a 5.57 hour binary system (Mason et al 1980, Mason and
Cordova 1982a, Mason et al 1932 and Mason and Cordova 1982b). The
ultraviolet observations were made with the IUE satellite and the infrared
observations with the NASA IRTF telescope on Mauna Kea. 2A 1822 -371 has
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proved to be an extremely important system for furthering our understanding
of the structurs of accretion disks around X-ray binaries and cataclysmic
variables and the orelationship between these two types of objects. The
light curve of the star varies as a complex function of energy. Evidence is
presented for a bulge on the outer edge of a luminous X-ray heated accretion
disk caused by the impact of the mass transfer stream From the companion.
The complexity of the ultraviolet, optical and infrared light curve is found
to be due to the fact that the modulation is made up of four components -
occultation of the luminous disk by the bulge, the changing aspect of the
X-ray heated inner face of the bulge, the changing aspect of the cooler
outer face of the bulge and the changing aspect of the X-ray heated face of
the companion (mass donating) star. Such a model fits the data extremely
well when model parameters are used that are consistent with the X-ray light
curve. This source provides the best measurement so far obtained of the
vertical structure of an accretion disk. The model also provides a distance
estimate of about 2.5 kpc for the star.
IUE ultraviolet observations have also been made of a number of
cataclysmic variables. Evidence of a high velocity wind has been discovered
in the dwarf nova TW Vir during its optical outburst state, in the form of a
marked P Cygni profile in the CIV 1549 line (Cordova and Mason 1982).
Observations of the eclipsing system RW Tri have also been obtained which
are consistent with this idea. It was found that the ultraviolet line
emission of this star did not diminish during the eclipse of the continuum,
indicating that the lines come from a large extended source. Time resolved
ultraviolet spectrophotometry has also been obtained on the pulsating
cataclysmic variable H2252-035. No modulation corresponding to the 3 hour
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Publications
1 A 5.57 hour modulation in the optical counterpart of 2S 1822-371
(K.O.Maaon, J.Middleditoh, J.Nelson, H.White, P.Seitzer, I-Tuohy
and L.K.Hunt) 1980, Ap.J. 242, L109.
2 4U 1626-67: A prograde spinning X-ray pulsar in a 25003 binary
system (J.Middleditch, K.O.Mason, J.Nelson and N.White) 1981,
Ap.J. 244, 1001.
3 An optical burst from the star associated with 2S 1254 -690
(K.O.Mason, J.Hiddleditch, J.Nelson and N.White) 1980, Nature
287, 516.
4 A soft X-ray halo around SU UMa (F.A.Cordova and K.O.14ason ) 19809
Nature 287, 25.
5 A soft X-ray survey of selected cataclysmic variable stars with the
Einstein observatory (F.A.Cordova, K.O.Mason and J.E.Nelson) 1981
Ap.J. 245, 609.
6 Pointed soft X-ray observations of AM Herculis from HEAO-1
(I.R.Tuohy, K.O.Mason, F.Lamb and G.Garmire) 1981 Ap.J. 245,
183.
7 Identification of the X-ray source E 1551+718 with an uncatalogued
dwarf nova (K.O.Mason, G.A.Reichert, S.Bowyer and J.Thorstensen)
1982 PASP (in press)
8 Ultraviolet spectrophotometry of 2A 1822-371: A bulge on the
accretion disk (K.O.Mason and F.A.Cordova) 1982 Ap.J. 255 9 603.
9 Phase resolved optical spectroscopy of the compact X-ray binary 2A
1822-371 (K.O.Mason, P.G.Murdin, I.R.Tuohy, P.Seitzer and
G.Branduardi-Raymont) 1982, MNRAS 200 9 793.
10 Optical identification of the X-ray source E1405-451: a 101.5
minute binary system with extremely rapid quasi-periodic
variability (K.O.Mason, J.Middleditch, F.A.Cordova, K.A.Jensen,
G.Reichert, P.G.Murdin, D.Clark and S.Bowyer) 1983 Ap.J. 264 (in
press).
11 Infrared photometry of the X-ray binary 2A 1822-371: A model for
the Ultraviolet, Optical and Infrared light curve. (K.O.14ason
and F.A.Cordova) 1982, Ap.J. 262 (in press).
12 High velocity winds from the accretion disk of a dwarf nova in
outburst (F.A.Cordova and K.O.Mason) 1982 Ap.J. 260, 716.
13 Ultraviolet observations of the X-ray binary pulsar H2252-035 (
F.A.Cordova, E.Fenimore , J. Middleditch and K.O.Mason) 1982
Ap.J. 265 (in press).
f
14 Observations of quasi-coherent soft X-ray oscillations in U
Geminorum and SS Cygni (F.A.Cordova, T.J.Chester, K.O.Mason,
S-M-Kahn and G.P.Garmire 1983 Ap.J. (in press).
15 X-ray observations of a large sample of cataclysmic variables stars
using the Einstein X-ray observatory (F.A.Cordova and K.O.Mason)
1983 Ap-J. (to be submitted).
16 Accreting degenerate dwarfs in close binary systems (F.A.Cordova
and K.O.Mason) in Accretion driven stellar X-ray sources ed.
W.H.G.Lewin and E.P.J.van den Heuvel, Cambridge University Press,
Cambridge, England (1982).
17 Cataclysmic variable stars from X-ray to infrared wavelengths:
Recent results on the continuum distribution (F.A.Cordova and
K.O.Mason) IAU Commission No.27 on variable stars, ed. D.Fernie
(1982).
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The nautre of dwarf novae and related systems

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