http://www.cnr.it/ontology/cnr/individuo/prodotto/ID5697
BeppoSAX observations of two unclassified LMXBs: X1543-624 and X1556-605 (Articolo in rivista)
- Type
- Label
- BeppoSAX observations of two unclassified LMXBs: X1543-624 and X1556-605 (Articolo in rivista) (literal)
- Anno
- 2003-01-01T00:00:00+01:00 (literal)
- Alternative label
Farinelli R., Frontera F., Masetti N., Amati L., Guidorzi C., Orlandini M., Palazzi E., Parmar A.N., Stella L., Van der Klis M., Zhang S.N. (2003)
BeppoSAX observations of two unclassified LMXBs: X1543-624 and X1556-605
(literal)
- Http://www.cnr.it/ontology/cnr/pubblicazioni.owl#autori
- Farinelli R., Frontera F., Masetti N., Amati L., Guidorzi C., Orlandini M., Palazzi E., Parmar A.N., Stella L., Van der Klis M., Zhang S.N. (literal)
- Pagina inizio
- Pagina fine
- Http://www.cnr.it/ontology/cnr/pubblicazioni.owl#numeroVolume
- Note
- ISI Web of Science (WOS) (literal)
- Titolo
- BeppoSAX observations of two unclassified LMXBs: X1543-624 and X1556-605 (literal)
- Abstract
- Observations of two unclassified Low Mass
X-ray Binaries, X1543-624 and
X1556-605, are presented. In the 2-10 keV
band the first of the two
sources is a factor of two stronger than
the other. Both sources do not
show X-ray bursts, dips or eclipses in
their X-ray light curves. We find
that both spectra are described by a
two-component model consisting of
emission from a cool accretion disk plus a
Comptonized blackbody with
kT_{bb} ~ 1.5 keV in a low opacity plasma.
The spectrum of X1543-624
hardens from the first to the second
observation, when the source slowly
moves from right to left in the
colour-colour diagram. The spectrum of
X1556-605 can also be described by a model
consisting of a blackbody plus
an unsaturated Comptonization with electron
energy kT_{e} ~ 4 keV. In the
first observation, X1543-624 shows evidence
of a Fe K emission line at 6.4
keV. Moreover, in both observations, the
source spectrum exhibits an
emission feature around 0.7 keV, which is
interpreted as due to the
superposition of the K edge absorption
features of O and Ne elements with
uncommon relative abundances with respect
to the solar one (O/O_{sun} ~
0.3, Ne/Ne_{sun} ~ 2.5). In the spectrum of
X1556-605 no emission lines
are observed. We discuss these results and
their implications for the
source classification and the accretion
geometry of the compact object. (literal)
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