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Set against the background of beautiful Mirabello Bay, astronomers
from fourteen countries met at Elounda, Crete in the period
7-18June, 1999 to debate some of the most compelling issues of
present day astrophysics. Neutron stars and black holes have been
at the forefront of astrophysics for over thirty years. As recently
as ten years ago it was still being debated whether galactic
stellar-mass black holes existed or not.It is now generally
accepted that many (possibly a thousand) stellar-mass black holes -
most of them still undetected - lie in low mass X-ray binary (LMXB)
systems; a few of them are detected every year as X-ray or
gamma-ray transients. These objects are more massive than 3 M, the
maximum possible mass 0 for a neutron star, and show none of the
tell-tale signs of neutron stars, such as X-ray bursts and X-ray
pulsations. It is quite remarkable that all LMXBs display a similar
temporal and spectral behaviour, 'independently of whether the
accreting compact object is a neutron star or a black hole. A broad
debate on these similarities and differences naturally constituted
one of the main focal points during the Elounda meeting. Evidence
on these aspects has been forthcoming from the Compton Gamma-ray
Observatory (CGRO), the ROSAT and ASCA satellites, the Rossi X-Ray
Timing Explorer (RXTE), and from the Beppo SAX Observatory."
Set against the background of beautiful Mirabello Bay, astronomers
from fourteen countries met at Elounda, Crete in the period
7-18June, 1999 to debate some of the most compelling issues of
present day astrophysics. Neutron stars and black holes have been
at the forefront of astrophysics for over thirty years. As recently
as ten years ago it was still being debated whether galactic
stellar-mass black holes existed or not.It is now generally
accepted that many (possibly a thousand) stellar-mass black holes -
most of them still undetected - lie in low mass X-ray binary (LMXB)
systems; a few of them are detected every year as X-ray or
gamma-ray transients. These objects are more massive than 3 M, the
maximum possible mass 0 for a neutron star, and show none of the
tell-tale signs of neutron stars, such as X-ray bursts and X-ray
pulsations. It is quite remarkable that all LMXBs display a similar
temporal and spectral behaviour, 'independently of whether the
accreting compact object is a neutron star or a black hole. A broad
debate on these similarities and differences naturally constituted
one of the main focal points during the Elounda meeting. Evidence
on these aspects has been forthcoming from the Compton Gamma-ray
Observatory (CGRO), the ROSAT and ASCA satellites, the Rossi X-Ray
Timing Explorer (RXTE), and from the Beppo SAX Observatory."
This slide presentation reports on the current status of Magnetar
observations, and on the results combining multi-satellite.
Magnetars are magnetically powered neutron stars. There is
discussion about several Soft Gamma Repeaters (SGR) also known as
Magnetars, though there aer other neutron stars that may be
considered as magnetars (i.e., Anomalous X-ray Pulsars (AXPs) Dim
Isolated Neutron Stars (DINs) Compact Central X-ray Objects (CCOs)
Rotation Powered Pulsars.) An example of a Rotation Powered PSRs,
(i.e., PSR J1846-0258) is reviewed, and examples of SGRs are
reviewed (i.e., SGR 0501+4516, SGR 0501+4516, SGR J1550-5418, and
SGR 0418+5729). There is also discussion about Photospheric Radius
Expansion (PRE) in thermonuclear bursts.
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