MASIVE
X-RA
New
Y
devlopmnts
BINARES
in
Ignacio
the
INTEGRAL
er
a
Negurla
artmeno
A
Dep
de
lic
ante,
F
P.O
sic
a,
Box
Ingeir
9,
E038,
a
de
A
lic
Sistema
y
ante,
Sp
T
e
or
a
de
la
Se
nal,
~
Universda
de
ain
[email protected]
Abstrac
The
study
of
masiv
diagnostc
the
ev
of
more
y
p
whic
h
In
e
yp
blac
k
y
p
h
repsn
the
relativ
ma
t
y
ears,
y
of
jor
our
sub
ject
v
y
X-ra
for
the
olv
ed.
in
com-
erd
a
absor
new
ed
and
h
v
ws
disco
b
resac
and
in
asumption
of
{
has
harcteisd
previous
thre
hanism
gro
,
c
as
the
than
picture
INTEGRAL
h
star,
formatin
mec
this
binares,
e
their
ysical
erd,
ationl
suc
More
of
ph
v
observ
masiv
ces.
picture
the
disco
pulsar:gen
sp
ec-
guarn
near
tes
futre.
ys:binare
er,
b
can
imp
a
t
vide
for
list
of
on
e
MXBs
pro
ertis
binary
of
vide
,
olutin
agin
binary
ev
and
b
y
they
and,
on
star
pro
galxies,
Finaly
ev
ts
neutro
(e.g,
consider
203).
constrai
is
winds
when
al.
ters,
question,
stelar
age,
et
in
tal
oung
an
star
ysical
of
y
of
(neutro
fundame
struce
of
wn
er
their
strong
formatin
kno
b
masiv
vide
osed
ject
astroph
um
Grim
of
the
of
comp
ob
informat
(cf.
pro
source
higest
n
the
of
phase
can
t
to
ecaus
pro
ortan
whole,
the
a
rates
hanism
recn
of
adres
star
v
y
compat
jects
to
X-ra
acreting
ob
us
formatin
an
are
an
neutro
star
ely
a
are
ws
they
their
mec
o
(MXBs)
of
as
A
e
and
More
t
and
b
Thes
mase
consider
w
some
star
alo
opulatin,
as
t
X-ra
of
pro
cohern
t
isue,
winds
acretion
a
are
e
binares
e
198).
a
and
to
ortan
ysical
stelar
of
halengs
wil
masiv
hole).
the
jects
last
imp
astroph
duction
study
er
suc
the
{
X-ra
e
their
as
this
tro
Masiv
early-t
Kap
c
the
led
masiv
vides
tal
star,
sytem
er
binares:clo
1.
from
Ov
e
pro
fundame
understaig
more
of
tha
as
some
opulatin
tra,
or
.
v
binares
of
ob
and
plexit
er
e
ha
and
As
y
b
masiv
study
olutin
X-ra
um
compat
of
ev
n
of
decas
ords:
a
olutin
formatin
Keyw
e
for
Liu
blac
et
olutin
k
al.
holes.
(20).
2
The
v
tron
ast
ma
star)
jorit
y
and
of
can
b
MXBs
e
c
con
tain
X-ra
harcteisd
b
y
y
the
pulsar
(magnetisd
pulse
or
neu-
spin
p
erio
d
P
.
F
or
s
a
few
MXBs,
searc
X-ra
hes.
Some
presnc
of
of
an
ramets
pulse
a
d
F
um
are
er
of
y
signca
detc
y
y
c
hole
The
of
the
et
b
trel
p
obtained
one
et
erio
ds
al.
(
1978).
e
comp
Quain
in
al.
only
optical
orbital
pa-
shift
ort
can
in
orbital
Dopler
Rap
(cf.
thorug
candites.
solutin
MXBs,
of
of
1972;
ties
of
k
anlysi
al.
hanges
uncertai
fraction
blac
spite
detrminao
via
et
cit
d
the
sytem
hrei
elo
in
o
ed
orbital
man
t
w
detc,
v
b
a
alo
Sc
radil
aectd
or
b
(e.g,
of
e
go
has
n
pulsation
b
consider
pulsar
times
anlysi
metho
are
y
al
no
from
canot
them
large
ariv
When
pulsation
X-ra
for
the
y
ts,
a
203).
P
)
are
kno
wn
orb
one
o
throug
dict
y
tha
of
in
the
the
the
metho
X-ra
p
ds
y
ositn
ligh
describ
ed
tcurv
of
e.
an
ob
F
ject
ab
or
o
X-ra
in
v
e
y
the
or
b
ecaus
of
pulsar,
Corb
P
/
P
a
et
clear
p
(1986)
diagrm
eri-
found
corelats
w
el
s
orb
other
a
with
n
ph
um
b
thre
er
ysical
of
pro
ertis.
MXBs.
Ob
Suc
jects
h
are
a
diagrm
observ
is
ed
to
sho
wn
dive
in
Fig.
rathe
1
for
cleany
in
to
groups.
MXBs
with
short
P
(a
few
second)
and
short
P
(a
few
da
ys)
s
orb
38
are
observ
ed
as
v
ery
brigh
t
(
L
1
10
erg
s
)
p
ersitn
t
X-ra
y
X
source.
It
an
is
b
acretion
Ro
eliv
ed
disk
c
he
lob
hanced
e,
tha
and
mater
tha
thoug
is
the
mas
b
mas
is
p
eing
transfed
donr
erhaps
throug
is
close
to
transfed
ling
its
throug
an
en-
wind.
Only
a
X-3),
few
suc
one
h
in
X-4).
sytem
the
SMC
Another
the
k-hole
ery
o
v
ero
w
nes,
and
stil
w
to
I
I
ery
Ho
h
v
ev
e
lo
b
er,
b
eliv
to
to
of
e
(Cen
ed
ed
ecaus
b
y
(LMC
eliv
b
Ro
c
v
b
e
a
e
brigh
erd
e
in
he-lob
their
disco
\clasi"
t-
and
it
is
MXBs.
v
oks
e
lik
en
a
LMC
b
catsrophi
ha
whic
ha
b
to
as
the
is
are
MXBs
them
W
in
efor
w
rst
Milky
one
jects
sytem
they
the
X-1)
ob
rae.
thes
X-1,
,
compat
MXBs
v
to
in
Probaly
the
e
ref
SMC
t).
Thes
the
donrs
(excpt
gian
of
b
to
mas
I
The
and
b
among
in
(LMC
imedatly
er
customary
one
LMC
t.
phase
so
thes
the
alen
ed
wn,
X-1)
in
equiv
short-liv
kno
(SMC
sytem
blac
v
are
sw
luminost
y
e
a
olen
lo
b
clase
around
w-luminost
y
y
the
gra
sup
er-
vitaonl
pul
compani.
with
long
P
(h
undres
of
second)
and
relativ
ely
short
P
s
orb
36
are
observ
ed
as
mo
deratly
brigh
t
(
L
10
1
erg
s
)
p
ersitn
t
X
X-ra
y
terpas
source
with
are
b
sup
are
ergian
eliv
alw
a
t
ed
a
on
to
ys
b
to
large
the
e
OB
degr
due
sup
of
ergian
neutro
to
direct
ts.
v
The
ariblt
y
observ
from
withou
The
optical
ed
acretion
star,
.
a
c
stable
the
coun-
harcteis
wind
acretion
of
the
disk.
Masive
X-r
ay
binares
Ther
3
are
10
of
conrmed
thes
sytem
furthe
and
noe
candites.
in
Becaus
the
of
X-ra
y
in
Cyg
coun
Binares
Galxy
Ther
SMC.
their
the
,
is
X-1
w
terpas,
one
ould
b
thes
with
couple
of
candite
e
in
the
ob
a
blac
jects
k
are
un-
the
hole
LMC
equiv
caled
alen
Sup
t.
ergian
t
(SXBs).
MXBs
with
Be
coun
terpas
ha
v
e
relativ
ely
long
P
.
They
p
op-
orb
ulate
a
rathe
naro
w
region
of
the
P
/
P
diagrm,
in
spite
of
s
orb
the
fact
ha
tha
their
viours.
A
X-ra
y
subtan
ligh
tial
tcurv
n
um
es
b
er
sho
of
w
a
thes
h
ob
uge
div
jects
ersit
y
are
of
X-ra
b
y
e-
tran-
3
sien
ts,
sho
e.g,
wing
v
Campn
ery
lo
et
w
al.
X-ra
y
20)
uxes
and
in
quiescn
luminoste
close
38
limt
for
a
Thes
neutro
star
sytem
Only
a
gories:
are
few
kno
among
the
w
quasr
el
2E
erg
as
<
to
1
10
erg
the
s
;
Edingto
1
10
wn
the
micro
(
(
s
)
Be/X-ra
y
studie
during
brigh
binares
MXBs
fail
0236.+1,
t
outbrs.
(BeXs).
to
whose
t
coun
in
to
thes
terpa
cate-
is
the
B0
V
e
Æ
star
LS
I
whose
+61
30
coun
and
(Masi
et
terpa
the
p
is
eculiar
al.
the
204),
the
wind
O6.5
V(f
acreto
micro
)
4U
quasr
star
LS
RX
5039
206+54,
J1826.
(Rib
iden
o
tied
1450,
et
al.
with
20),
the
p
eculiar
Æ
O-t
yp
e
star
BD
Another
+53
p
part
is
of
ob
the
eculiar
indcate
v
CI
eculiar
Cam
is
ev
whose
a
B[e]
are
stage,
sup
ergian
w
t
ould
optical
star
olutinary
J0421+56
201).
J0421+56,
Thoug
t
Reig
sev
(Hynes
b
e
a
coun
motley
eral
et
then
a
lines
al.
of
20,
argumen
and
MXB,
ev
ter-
groupin
en
t
refncs
thoug
a
v
ery
one.
2.
The
The
Be/X-ra
clas
the
of
mas
BeX
the
In
also
b
e
a
y
of
w
pro
a
ecaus
(se
BeXs
ertis
&
micro
could
the
fact
a
a
of
materil
for
a
recn
0236.+1
discuon
w
a
the
y
of
displa
y
ph
t
could
genral
this
tha
(someti)
disk
203,
2E
doubt
y
star
y
Rivnus
for
in
one
e
quasr
den
tha
masiv
b
205,
er,
b
suronde
orte
the
Negurla
ev
ely
is
P
sen,
den
relativ
it
itself
(se
Ho
simply
i.e,
b
genral
BeX
genraly
star,
star
this
denito).
ariet
Be
lines
from
reviw).
is
a
emison
eld
binares
binares
is
ting
exp
y
donr
presn
v
XTE
Cam.
diern
XTE
p
CI
ery
tha
therin).
&
is
star
in
(Negurla
sytem
B[e]
jects
2790
ysical
suc
h
realit
a
the
y
h
uge
of
this
groupin.
Most
BeX
erio
ds
ysical
sytem
of
are
transie
quiescn.
A
mec
hanism
details
sytem,
the
ph
p
are
w
e
presn
leading
stil
observ
ts
t
to
e
o
relativ
to
ying
w
this
complex
quic
e
b
to
ely
displa
t,
b
eha
alo
(a
tha
at
acurte
few
y
e
viour
w
k
X-ra
eliv
outbrs
and
w
the
e
the
basic
lev
el,
predictons.
y
ears)
thoug
In
quasi-p
long
understa
erio
dic
sev
eral
cyles,
triangle
star,
Figur
e
BeX
1.
is
SAX
sytem
The
J2103.5+4
P
orb
are
/
P
s
triangles
plot,
a
The
mo
and
dern
led
sup
v
ergian
ersion
cirle
t
is
of
sytem
the
the
p
diagrm
eculiar
are
square.
transie
from
Corb
The
t
A
et
led
0538
(1986).
square
6.
Clasic
Se
is
the
the
tex
h
masiv
yp
ergian
for
e
discuon.
X-ra
t
binary
y
binares
GX
301
are
repsn
02.
The
ted
led
as
4
Masive
X-r
T
able
ay
1.
clas
P
t
Reig
v
w
BeX
&
binares
slo
5
ersitn
(after
BeX
binares
with
c
slo
pulsation
is
candites.
he
The
19).
w
and
aribles
and
Ro
The
pulsation,
no
w
ob
o
ob
the
coun
p
t
while
detc
marginly
four
rst
jects
in
other
terpa
in
jects
the
an
den
are
Galcti
iden
the
panel
are
so
panel
second
thre
(and
top
the
ob
ticaon
SMC
jects
as
with
catlysmi
osible).
Ob
ject
P
(s)
s
X
P
er
J0146.9+2
RX
J04.9+31
RX
J1037.5
835
RX
140
20
AX
J049.5
AX
J013
5647
732
whic
X-ra
y
y
w
and
the
the
(Ok
&
a
c
siten
los
four
BeX
BeX
v
gro
ws,
Negurla
b
star,
et
y
a
v
the
w
en
giv
et
ernd
Be
displa
ose
ery
es
al.
rise
Reig
in
of
neutro
to
201;
complex
dynamics
the
the
t
fol
while
h
terpla
the
star
a
most
les
X-ra
up
c
er
y
v
panel
y
Be
and
disk
the
ariblt
disk
y
of
harcteis
T
able
.
Based
1),
diern
transie
alw
s,
uc
the
wing
BeX
sytem
20
m
in
from
ersitn
ys
(listed
binares
>
(e.g,
go
b
pulsar
pro
P
forms,
201).
(19)
P
star
ears
teracion
of
of
(1)
Be
the
Negurla
sample
t"
715
the
from
group
he
20
419
are
in
smaler
on
J170
cyles
vitaonl
azki
A
AX
437
275
disap
h
mas
gra
J1749.2
then
Suc
en
AX
594
around
and
345
J1452.8
disk
201).
et
Ro
the
activ
al.
b
et
h
756
72
1SAX
during
862
Reig
&
tiang
\p
er-
ys
ts:
displa
y
transie
relativ
ts
ely
ha
v
e
long
pulse
shorte
p
p
erio
erio
ds,
ds.
s
35
1
<
(2)
P
ersitn
t
source
alw
a
ys
displa
y
lo
w
X-ra
y
emison
(
10
erg
s
)
with
smal
sien
smo
oth
uctaions,
compared
to
the
outbrs
of
tran-
(3)
ts.
The
X-ra
y
ergy
(
dep
sp
4
ectra
k
endc
(4)
X-ra
y
at
w
eakly
,
6.4
.
k
sp
eV
p
ersitn
t
compared
on
The
line
of
eV
in
to
tensi
ectra
y
tha
of
is
presn
20
k
ts
eV
in
a
lo
w
cut-o
transie
en-
ts)
and
no
.
p
genraly
source
10
ersitn
sen
t
source
in
do
transie
es
ts,
not
or
sho
sho
w
ws
the
it
iron
v
ery
6
Other
X-ra
(second
y
pulsar
panel
are
of
BeX
able
c
The
tha
0726
e
et
en
eha
v
es
a
e
no
w
o
the
of
ersitn
clas
AX
J013
72
harcteis.
t
coun
this
and
c
p
X-ra
y
terpa
source
and
ther
is
binares.
is
t
t
ers
denig
optical
groups
ersitn
b
732
of
tly
e
me
J049.5
y
apren
p
b
catlysmi
t
the
as
v
realy
the
to
b
AX
apren
ha
are
w
to
man
are
excptions
260
osed
them,
they
they
b
b
pro
sharing
but
hance
to
en
candites
divson
sem
b
SMC
pulsation,
smal
e
Among
the
Galcti
long
v
1).
in
thre
with
X
T
sytem
The
a
ha
not
sharp
rules.
and
F
source,
but
or
inde
ther
instace,
has
the
P
=
103
s
source
(Corb
et
&
s
P
el
197).
tha
A
b
oth
t
fundame
yp
tal
es
of
BeX
comnalit
y
sytem
o
cup
w
y
ould
b
the
e
indcate
same
b
region
of
y
the
the
fact
P
/
P
s
orb
As
b
diagrm.
et
w
en
rst
P
noticed
and
b
P
for
y
Corb
et
BeX
(1984),
ther
binares.
The
is
a
clear
corelatin
corelatin
is
not
tigh
t,
and
s
orb
a
few
sytem
not
J1946+27
ha
XTE
do
v
e
sem
(Wilson
a
observ
ed
L
fol
et
demonstra
and
w
al.
hig
P
a
it,
for
203).
of
large
exampl
Ho
degr
for
X
BeX
to
X
w
ev
er,
Ma
corelatin
b
sample
of
0726
jid
et
SMC,
260
w
et
en
al.
(204)
the
LMC
and
maxi
and
um
Milky
W
a
y
s
sytem,
something
tha
only
mak
es
sen
if
P
is
directly
corelatd
s
to
the
size
of
orbital
p
the
erio
sytem
d
orbit.
in
is
The
kno
the
wn,
P
only
/
X
P
P
p
ersi,
ersitn
t
fals
diagrm,
righ
and,
BeX
b
t
binary
b
et
w
ecaus
for
en
of
the
the
whic
h
transie
L
/
s
the
t
P
BeX
corelatin
X
s
orb
found
b
other
y
p
Ma
jid
et
ersitn
The
t
w
tha
as
in
the
v
corelatin
w
radius
erio
equals
the
of
to
an
angulr
v
the
to
the
an
elo
cit
exp
ect
tha
al
the
(se
elo
y
also
wind
the
w
spin
al.
up
b
e
They
conlude
the
tha
neutro
King
could
equi-
1986).
and
conlusi,
the
magnetosphric
et
out
could
this
The
conlude
at
at
Stela
w
1986).
rotaing
cit
neutro
et
who
star'
y
the
(Corb
(198),
slo
tum
fact
Kerkwij
neutro
Against
moen
reason
in
v
this
d.
d
spin
equatoril
from
o
lie
cortain
v
erio
go
ust
&
the
e
equilbrm
aters
due
as
p
enough
W
as
materil
equilbrm
tha
y
when
disk
v
same.
of
Keplrian
Be
acretion
this
d
the
del
the
kind
b
p
ha
m
some
estigad
spin
do
e
corelatin
at
librum
mo
this
rotaing
isue
w
to
for
is
(204),
source
reason
star
al.
star
suplied
(19)
to
doubte
throug
this
mec
ha-
nism.
On
the
diern
other
t
(198).
from
e
y
(Ok
no
b
y
e
&
aski
mo
tha
ts
(se
angulr
y
W
the
aters
disk
&
v
is
an
azki
201).
detail
mo
inde
dels
P
is
h
to
in
observ
y
can
neutro
azki
ed
b
disk
the
Ok
ery
held
Suc
tum
v
Kerkwij
and
moen
and
Be
quasi-Keplrn
Ok
of
204),
b
are
201;
amoun
azki
used
disk
disk
Ok
of
del
Be
acretion
&
understaig
Negurla
large
an
Ha
t
wind
eliv
azki
throug
20;
curen
radil
w
transfe
star
probaly
our
the
W
viscot
hand,
et
to
al.
decras
strongly
s
during
BeX
outbrs
(e.g,
Finger
et
al.
19;
Wilson
et
al.
Masive
X-r
T
able
ay
2.
XTE
e
7
Be/X-ra
y
J1543
b
binares
568
BeX
transie
ts
and
sytem
2S
b
with
153
ecaus
of
Ob
lo
542
w
ecn
are
their
trices.
The
actuly
not
transie
t
b
ject
eha
kno
optical
wn,
coun
but
terpas
they
are
to
b
eliv
ed
to
viour.
P
(da
ys)
e
orb
GS
0834
430
XTE
KS
153
sugetin
is
lik
tha
the
spin
up
and
spin
e
wn
et
y
:
25
40
:
42
0
:
02
30
:
60
2
:
20
se
also
40
0
<
0
:
17
<
0
:
03
:
09
0
:
03
<
angulr
0
moen
stem
tum.
from
an
materil
p
but
:
of
quiescn,
1986;
0
56
of
acretion
during
al.
:
realy
b
80
75
transfe
corelatin
caused
do
(Stela
542
ectiv
ely
the
:
568
1947+30
2S
203),
105
J1543
erhaps
b
angulr
caused
b
ort
et
it
equilbrm
with
Rap
Therfo
al.
et
w
en
moen
y
the
tum
pro
elr
ect
204).
>
Most
BeX
binares
ha
v
e
mo
derat
or
large
orbital
ecn
trices,
e
0
:
3.
Ev
only
olutinary
b
the
mo
e
explaind
if
neutro
P
star
ortegis
prot
art
yp
and
P
sup
p
sho
a
v
an
wn
tha
thes
explosin
cit
y
kic
el
X
v
et
P
an
can
w
but
is
P
er
al.
trices
symetric,
it
&
sytem
(Delgado-Mrt
ecn
not
when
Heuv
BeX
hig
are
elo
den
t
d
e
v
a
v
ersitn
250
v
erno
es
195;
e
=
ha
reciv
Zw
the
dels
b
orn
rathe
(Hab
ardijs
ets
197).
as
found
201).
to
Based
1987;
Ho
ha
v
on
w
e
e
ev
er,
=
this,
0
:
1
Pfahl
et
orb
(20)
c
al.
argued
tha
harcteisd
b
y
it
long
(
w
as
p
P
>
osible
to
30
d)
den
a
orbital
p
erio
new
sub
ds
clas
and
lo
of
w
MXBs
ecn
trices.
orb
As
the
o
long
orbital
cured
the
lo
a
w
sup
the
ecn
v
This
a
w
is
ev
y
Ok
is
a
go
&
p
ersitn
t
615,
X
P
can
b
diern
t
set
d
b
orbital
BeX
p
tha
ha
a
y
and
407
s),
y
ha
also
v
e
y
w
o
orbits
lo
transie
BeX
w-
t
v
e
for
lo
w
e
,
as
transie
e
This
casionl
w
h
mo
b
eha
del
viour
suget
tha
transie
lo
whic
the
t
.
ts
ecn
e
BeX,
are,
binares
ha
and
BeX
on,
Ther
hig
some
wide
in
tric
no
and
the
ely
e
formed
w-ecn
t
tha
relativ
e
parmets.
suget
ving
v
(from
ersitn
man
v
star,
ha
lo
clas
ma
sytem,
=
en
ust
four
ationl
e
(201)
P
w
ha
neutro
.
the
detrminao
to
kic
the
observ
eliv
a
sen,
et
of
m
y
and
e
the
sytem
er
b
distnco
relatd
18
y
As
Negurla
timaely
al
b
2.
canot
creatd
b
to
o
cirulaston
tha
the
den
able
a
tidal
explosin
acompnied
reason
not
azki
in
A
on
strong
is
e
T
the
based
er,
ther
b
in
acros
h
ho
ould
tha
a
primodal:
not
listed
cuts
imply
v
are
w
ts
whic
ds
erno
explosin
clas
BeX)
erio
sup
trices
erno
transie
b
p
after
(suc
h
as
trices.
s
A
KS
go
o
d
coun
terxampl,
1947+30,
ho
whic
h
has
w
P
ev
er,
=
is
40
:
pro
4
vide
d,
b
P
=
y
the
18
:
7
BeX
s
transie
and
t
e
=
0
:
s
03
orb
(Galo
w
a
y
et
al.
204).
This
ob
ject
has
sho
wn
a
v
ery
hig
lev
el
of
X-
8
Figur
e
KS
2.
Blue
sp
1947+30,
tak
rming
the
explain
B0
V
e
withn
ra
y
activ
y
More
v
to
sp
ectral
t
t
recn
er,
While
lo
w
e
,
lo
w-
568
y
the
.
star
tha
it
this
w
ob
(La
y
as
alm,
in
mas
of
'
16
and
ersi
.
ma
y
ust
t
diÆcult
to
yp
e
v
v
IS
er
sp
the
b
b
explain
sup
o
terpa
sp
the
ectrum
lo
of
WHT
ectrum
is
whic
extrmly
to
4.2-m
sp
h
w
cur
conlude
clasiton
The
a
basicly
only
coun
using
v
los),
with
can
clasiton,
the
erno
mas
who
20,
ectral
a
orn
(203),
A
21st,
diÆcult
to
optical
al.
e.
y
orbits
The
ery
binares.
due
en
wide
ectrogaph.
sp
to
e
h
v
b
is
ha
suc
V
b
is
BeX
explaind
phase.
B0
em
(201).
568,
e
orbit,
Negurla
induce
et
t
No
orde
b
y
Negurla
the
In
con-
cirula
&
of
tric
ergian
y
conrms
M
t
IS,
rathe
almost
azki
J1543
in
on
2
transie
+
are
formatin
m
ectral
and
Fig.
P
sup
sp
sytem
XTE
1947+30
obtained
BeX
WHT
wide,
Ok
the
ecn
b
Spain)
ed
X
y
of
for
the
the
of
as
the
4.2-m
this
its
b
tha
dels
studie
ely
w
of
del
as
mo
KS
as
lik
ject
P
pla
el
of
ters
w
spite
cirulaston
en
1947+30
the
of
mo
(al
Tidal
to
with
parmets
in
orbit
and
tric
terpa
20,
The
the
w
k
coun
21st,
ears,
as
e
optical
er
ork.
y
kic
J1543
ecn
KS
e.
t
withou
when
yp
curen
the
explosin
b
of
its
the
em
framew
t
withn
no
v
predictons
explain
XTE
No
curen
in
the
of
on
the
aginst
ectrum
en
dis-
imples
ecn
a
tric
y
of
KS
1947+30,
tha
one
ga
v
lite
e
birth
mas
the
e
a
b
tha
ruled
simlary
w
to
ould
the
(close
k
out
v
b
lo
elo
y
the
e
w
Chance
as
to
asume
of
the
cured
it.
erno
a
The
the
a
sup
withou
during
balnced
coindes
tha
o
lost
exactly
existnc
.
e
star
noe)
cit
y
w
v
neutro
to
kic
ha
k
to
XTE
not
hap
a
J1543
en
t
explosin
and
tha
e
due
sytem,
do
kic
alterniv
impulse
second
v
p
mas
ery
y
los
568,
wice.
v
osiblt
with
can
Masive
X-r
P
o
binares
dsialo
clas
lo
the
w-
v
star
et
e
elo
k.
cit
y
kic
ks,
kno
m
wn
they
co
v
The
er
a
coun
des
e
the
BeX
y
a
of
w
v
of
dal
neutro
recivng
b
a
e
justied
v
b
furtheing
the
distrbuon
with
a
ould
for
existnc
bimo
explosin,
erno
t
X-ra
ery
y
our
smal
a
kno
ph
ysical
wledg
of
binares
timescal
and
in
BeX
ed,
SXBs
are
Inde,
w
thes
ork
are
exp
ectd
the
is
sytem
stelar
unlik
n
ely
OB
um
to
sup
b
b
e
ergian
ers
v
ery
ts,
but
parmets.
donr
kno
170
olv
staicl
in
of
e
v
binares.
henc
range
4U
y
than
donrs
wide
to
w-
umeros
masiv
terpa
lo
t
mas
most
mo
instrume
smal
The
t
olutinary
n
rathe
t.
diern
usefl
ev
les
are
signca
to
ergian
the
h
tha
b
hanism.
sup
uc
sugetd
explaind
of
a
of
e
e
sup
mec
Becaus
b
due
henc
The
v
naturly
clas
formatin
3.
e
elctron-apu
the
and
ha
b
an
Therfo
MXB
(204)
can
in
reason
to
al.
BeX
formed
kic
9
wski
of
in
ay
wn
37,
is
with
probaly
an
HD
1539,
estimad
the
mas
of
58
O6.5
1
Iaf+
M
(Clark
et
al.
sp
20).
In
ectral
t
yp
comparisn,
e
the
B0.5
Ib
and
a
mas
donr
mas
in
in
the
V
23
ela
X-1,
28
HD
M
7581,
range
has
(Quain
trel
et
al.
in
a
203).
m
This
X-ra
uc
y
of
h
earli
the
mas
a
SXB
as
(cf.
its
ev
kno
wn
apro
uc
h
more
masiv
it
ximately
The
the
pro
ertis
the
is
a
bit
the
star
203).
on
detrmins
this,
e
Maedr
strongly
stau
of
y
m
&
end
olutinary
displa
a
Meynt
dep
Becaus
36
is
should
struce.
sytem
1539
stage
of
donr,
wind
HD
olutinary
y
and
L
tha
ev
luminost
rate
the
means
mas
los
surping
tha
same
X-ra
y
al
luminost
y
,
1
10
erg
s
.
X
Man
y
of
the
SXBs
sho
w
pulsation
with
long
P
,
genraly
a
few
h
un-
s
dre
second.
In
the
P
/
P
diagrm
(Fig.
1),
they
trace
something
s
orb
close
to
a
horizn
tal
line,
as
the
P
do
es
not
sem
to
b
e
corelatd
to
s
P
.
In
the
standr
scenario
(W
aters
&
v
an
Kerkwij
198),
it
is
b
e-
orb
liev
ed
tha
the
neutro
star
w
er
b
orn
with
shorte
P
,
but
during
the
s
lifetm
b
main-sequc
en
a
of
main-sequc
the
presn
O-t
neutro
star
w
er
yp
spun
t
e
do
donr
wn
star),
(whic
no
to
h
m
acretion
thes
ust
to
presn
t
ha
ok
v
e
orignaly
long
place,
P
and
b
the
ecaus
of
the
s
pro
elr
los
ect.
rates
the
increasd
cretion
of
and
When
donrs
suÆcien
mater
so,
mas
tly
is
the
pulsar
not
b
to
p
ermit
b
not
spun
sup
ectiv
acompnied
are
ecam
up
bac
y
ergian
e
lo
w
angulr
v
mas
but
of
to
their
acretion,
transfe
k
ts,
this
ac-
moen
alues
of
P
tum,
.
s
This
lac
of
qualit
b
particul
of
trinsc
k
oth
ectiv
y
spin
of
up
v
alue
e
the
and
angulr
moen
mas
transfe
spin
(Anzer
tum
&
do
mec
B
wn,
orne
tha
is
hanism.
lo
195).
transfe
SXBs
ok
In
lik
e
an
displa
random
the
probaly
clasi
w
y
alks
episo
in-
des
Bondi-H
around
yle
a
10
form
ulation,
acretion
materil
do
es
acreting
b
the
not
o
to
to
a
angulr
unable
acretd
pro
In
Fig.
1,
t
P
w
line
=
a
a
:
e
can
se
b
4
d
answ
al.
er
as
to
w
m
ed
the
h
of
realistc
refncs
uc
the
sign
More
and
ho
w
hanged
192).
19;
vide
therin)
angulr
moen
tum
wind.
traced
10
clear
Ruert
the
pro
sho
c
et
195;
to
can
ulations
uosly
(Matsud
Anzer
vide
from
tin
and
ect
tha
sim
con
wind
resp
disk
Early
tha
fast
with
acretion
star.
y
ely
tum
stable
neutro
tum
relativ
moen
and
the
&
a
angulr
large
instabl
to
straigh
from
enough
up
moen
acretd
e
directly
a
(Ruert
are
curs
\ip-o"
ulations
is
v
form
spin
of
sim
ha
dy
torque
presnc
the
o
t
y
and
w
al
o
sytem
the
P
whic
other
=
38
h
SXBs.
s
deviat
strongly
One
(Chakrbt
is
y
et
O
A
from
al.
O
1657
the
415,
193).
with
This
sytem
s
orb
has
displa
it
o
y
ed
cupies
an
This
b
sup
eha
in
des
as
14
spin
p
b
is
18
of
termdia
could
t,
=
episo
viour
ergian
M
long
e
p
ositn
leading
b
erhaps
et
w
to
en
b
y
(Chakrbt
relativ
y
et
the
ely
al.
MXBs.
donr
w
is
mas
In
tha
clasi
mas
lo
193).
sugetion
and
if
the
the
SXBs
explaind
sugetd
M
up,
a
late-B
estimad
this
for
case,
the
sup
it,
ergian
t
w
ould
b
and
e
on
its
the
wind
SXBs,
w
alo
b
A
second
=
bi-stal
rathe
the
415
:
6
d
slo
v
ery
=
er
the
op
10
s,
than
20),
of
other
,
it
al.
osite
the
al.
those
and
et
et
Unfortuaely
obscured
y
in
P
w
Vink
tum.
(Chakrbt
and
(cf.
moen
is
infraed
jump
and
angulr
deviats
1
y
densr
1657
sytem
P
e
the
of
O
in
The
of
transfe
O
detc
with
side
the
to
en
ol
ould
wing
terpa
b
coun
co
has
only
the
recn
tly
20).
directon.
It
longest
P
is
2S
014+65,
measurd
s
in
a
neutro
s
orb
star
(Hal
not
et
clear.
al.
It
20).
The
has
b
en
reason
for
sugetd
this
tha
p
extrmly
slo
erhaps
the
w
pulsation
neutro
are
star
w
as
b
orn
14
>
with
a
v
ery
hig
magnetic
eld
(
B
10
G,
t
ypical
of
a
magnetr)
and
spun
do
wn
b
Ther
is
y
the
no
pro
ob
elr
vious
ect
(Li
&
corelatin
b
et
v
w
an
den
en
Heuv
el
P
and
19).
L
for
SXBs,
in
X
orb
con
tras
to
simply
b
stau
what
e
is
due
of
to
the
observ
ed
the
n
mas
um
b
for
er
donrs
BeX
of
sytem.
SXBs
has
As
b
to
b
e
eing
to
o
noted
ab
smal,
as
detrmina
t
for
o
the
v
the
e,
this
ev
L
ma
y
olutinary
exp
w
ectd,
as
X
el.
It
is,
ho
w
ev
er,
curios
tha
no
sytem
with
P
>
15
d
is
kno
wn,
as
orb
one
w
and
ould
lo
in
mark
w
er
princle
ed
exp
X-ra
in
y
ect
other
sytem
Fig.
luminoste.
1
to
The
as
a
led
exist
notable
square.
with
broade
excption
This
ob
orbits
is
ject
has
GX
P
301
=
41
:
02,
5
d,
but
orb
it
presn
ts
meanig
t
w
o
tha
phase
singularte.
ther
(with
is
the
fact,
us
ha
episo
v
des
a
h
v
v
hap
up
a
v
in
shortly
v
hig
e
a
b
mas
en
v
ery
y
p
blue
h
tric
ux
efor
los
observ
ecn
X-ra
b
is
ery
ha
is
ariton
terpa
and
spin
orbit
enig
coun
radius
rapid
its
large
optical
uge
of
ery
um
the
e
a
maxi
Second,
th
20).
First,
with
yp
t,
As
this
:
46,
Leah
y
and
a
sytem
0
orbital
cf.
ergian
in
=
the
eriaston;
rate.
ed
e
m
mater
ust
of
(Koh
Masive
X-r
et
al.
ay
binares
197),
GX
sup
301
the
1
02
idea
orting
is
th
tha
4.
the
us
The
t
genral
pro
Filng
the
P
/
a
man
y
transie
t
sen
are
from
acretion
disk
other
diÆcult
to
forms.
SXBs,
den
reinfocg
for
this
group.
gaps
of
in
tha
in
ertis
the
separtion
clear
idea
diern
MXBs
in
P
to
thre
diagrm,
distnc
but
groups
directly
is
not
conetd
only
to
v
the
ery
diern
t
s
orb
ph
ysical
mec
hanism
lutionary
in
stau
of
Among
A
w
0538
,
sion
in
unclear.
optical
I
I
I;
:
6
d
y
v
b
erio
the
t
source
is
In
sen,
ev
its
&
a
6
w
and
v
the
an
ev
o-
the
y
the
c
clasi
al.
in
(1986),
stage
the
ac-
pro
donr
at
0538
y
ose
mas
is
p
6
(via
as
b
ject
A
a
harcteisd
h
ob
MXB
er-
acompnied
to
whic
e
(sup
w
,
(1983)
compat
yp
emis-
t
source
y
ectrum,
binary
et
with
dict
et
Corb
t
H
brigh
erio
BeX
ectral
strong
When
the
a
outbrs
Charles
when
b
(sp
p
sp
t
as
ys
optical
same
tric
e
transie
extrmly
203).
the
ecn
lob
LMC
clased
luminos
ying
lead
ery
the
en
displa
emison
he
ard
ery
is
Charles
discue
to
of
and
displa
complex
c
as
olving
ces
b
v
0538
This
Ro
ositn
20)
with
ely
its
this
sytem
A
en
a
p
not
e
source,
cured
of
lik
ls
tron.
Co
proles.
casionly
a
w
P-Cygni
the
o
er,
(McGo
elopmn
pro
someti
is
y
o
strong
tha
ev
X-ra
outbrs
dev
ery
y
y
the
terpa
w
t
dict
X-ra
transfe
has
&
Ho
p
e,
mas
only
Negurla
transie
tiv
the
sytem
coun
cf.
quiescn.
Edingto)
16
in
This
its
B1
ed
sytem,
is
as
around
olv
sytem.
el-studi
6
binary
v
the
erias-
could
b
e
cirulaston
of
orbit).
The
X-ra
197
w
y
as
source
SAX
found
to
J2103.5+4,
fal
disco
righ
t
among
the
v
SXBs
erd
b
in
y
the
Bep
oSAX
P
/
P
in
diagrm
s
orb
in
spite
of
optical
b
eing
coun
al.
a
Its
1,
p
thoug
a
olutin
a
or
the
BeX-lik
e
shorte
subtan
y
tial
star
n
and
a
duce
w).
et.
If
um
b
If
the
ers
in
of
ev
olutin
an
e
v
b
they
O6.5
5039
V
the
star;
OB
its
star
a
turns
y
v
t
b
it
as
is,
a
bac
b
k
sup
e)
to
ect
they
an
to
to
a
tha
main-sequc
reason,
y
for
ed
can
luminost
spin
ypical
eliv
bring
OB
tly
the
alue
detc,
in
recn
case,
a
normal
it
in
the
only
this
to
not
et
triangle
are
some
X-ra
In
one
y
for
led
to
coret,
its
withn
SXBs
able
are
is,
.
,
(Reig
explaind
it
of
en
b
but
a
tly
star
has
y
ds
e
y
e
donr
caried
erio
formed
exist,
of
v
p
Be
b
b
is
(LS
is
ha
Recn
mild
ed
mas
terpaion
binares
e
activ
spin
ha
20).
V
erhaps
oradic
ould
not
this
emison
star
w
al.
B0
the
sp
the
could
star
y
ery
star
y
p
tha
v
et
a
mark
asume
(as
neutro
X-ra
optical
lo
e
al
as
diagrm,
ys
activ
spin
the
displa
sytem
and
the
w
yk
tied
can
neutro
no-acretig
pro
in
if
star
of
(Ba
iden
surping,
ork
Be
source
en
ositn
framew
ecom
ev
b
certainly
standr
b
t
has
204a).
Fig.
transie
terpa
ho
Be
do
not
excption,
as
star,
w
ev
er,
acretion
rathe
12
wil
star,
and
it
wil
mo
v
e
from
a
P
of
sev
eral
h
undre
second
to
the
s
equilbrm
p
ositn
coresp
ondig
to
its
P
.
If
the
OB
star
do
es
not
orb
displa
y
and
Be
ev
c
olv
e
harcteis,
it
to
w
Another
ard
the
sup
sytem
stage
in
ev
with
tha
MXBs
is
has
b
un
til
it
b
egins
to
sw
el
stage.
found
of
INTEGRAL
hiden
t
tly
olutin
remain
ergian
recn
the
tecd
wil
ma
IGR
en
y
repsn
t
an
J037+612.
iden
in
termdia
This
tied
with
1RXS
source,
de-
J0379.6+12,
Æ
a
R
OSA
T
Observ
source
coinde
ations
0
:
06
with
d.
displa
t
The
RXTE
ys
eak
the
/ASM
source
w
with
is
catlogued
rev
hardly
OB
eal
a
clear
detc
outbrs
with
p
erio
during
this
p
erio
star
BD
dict
y
most
dict
y
of
(den
+60
of
73.
15
the
:
65
time,
Hartog
and
et
al.
204).
Æ
Optical
observ
ations
(Negurla
of
&
sion
lines.
a
Reig
y
far
to
compat
ev
ject
the
in
B
w
to
v
olutinary
ha
v
stage
the
a
lik
e
a
Be
yp
comes
ery
to
tha
of
A
of
0538
to
w
e
tha
the
sur-
repsn
Ob
sytem
I
of
b
ould
6.
this
source
close
w
I
has
could
v
I-
emis-
and
The
othesi
J037+612
parmets
I
star
wind.
h
BN0.5
of
not
ely
orbit
IGR
yp
indcatos
stelar
a
tric
orbital
t
no
is
strong
case,
previous
of
ectral
terpa
e
ecn
sp
and
but
this
a
205),
clear,
ery
In
eal
al.
coun
not
a
star.
detrminao
imp
lo
rev
et
optical
is
ob
of
an
o
acretd
face
73
Reig
the
materil
a
+60
204;
Therfo
luminost
the
BD
t
viously
,
ould
b
e
the
of
hig
ortance.
5.
The
The
y
w
observ
and
o
w
era
INTEGRAL
X-ra
t
new
y
ard
telscop
no
.
y
thes
emison
the
sion.
the
An
y
up-todae
,
ha
list
of
v
the
e
new
htp:/isdcul3.nge
b
F
are
k
sp
X-ra
ept
b
y
y
w
rst
as
suc
observ
ed
materil.
h
to
sytem
b
Observ
e
as
w
m
uc
&
ra
(Mat
h
y
as
higer
v
y
the
in
a
ery
of
a
emison
is
J.
mis-
Ro
driguez
as
v
elop
at
ed
w
ed
of
of
in
h
ject,
for
undetcabl
terv
enig
phot
tha
elc-
directon
it
aso
searc
in
h
materil
tha
materil
ob
y
the
y
sugetion
e
.
whic
absoring
densit
the
b
tha
t
l
48,
absor
amoun
The
redn
J1638
sho
column
203).
ery
w
the
to
al.
IGR
ux
tha
en
v
as
sateli
tersla
dens
et
v
soft
eral
leading
in
disco
w
and
(Revnits
the
detc
its
203),
star
e
sev
lite
htm
ecaus
arible
than
imersd
to
b
b
with
Guainz
binary
donr
led
hard
ations
absorptin
w
tric
to
fre-
previous
rodigue/htmlsc.
The
ery
with
b
k
last
to-
ectra,
soft
is
the
v
detc
source
tains
ecialy
monitred
of
en
or
esp
hard
lac
not
con
source,
rathe
This
ha
20,
203).
y
h
e
er
al.
whic
v
ys.
they
Octob
X-ra
Galxy
X-ra
wh
new
source
soft
reason
in
et
eral
the
new
in
probaly
hed
Winkler
sev
of
of
launc
(se
detc
regions
Man
,
es
has
iner
tly
or
y
it
the
quen
-ra
ears,
atory
w
the
ciated
as
an
X-
with
coun
the
terpa
in
opti-
Masive
X-r
cal
ay
bands,
binares
ob
but
ject
rev
lines
rathe
eal
strong
ted
ondig
Chat
y
Ther
XTE
to
204)
is,
w
ev
terpa
caused
b
y
a
k
tly
acterisd
b
arc
hiv
al
y
disk
sp
et
al.
conrmed
b
P
=
y
to
of
s
(Luto
kno
wn.
h
terpa
yp
to
othesi
tha
hig
eral
them
absorptin
other
ha
b
of
v
e
source
later
en
c
b
other
en
observ
an
ed
with
ASC
.
Its
leading
MXBs.
Its
an
in
Among
pulsar,
is
har-
found
sateli.
acreting
it
al.
the
the
with
tha
et
source
to
sev
in
v
(Filatre
coun
tha
erd
of
pulsation
vino
emison
ts
other
(204)
past
tha
detcion
130
y
suget
of
this
it.
the
to
of
ealth
optical
and
previously
simlar
(203)
y
v
Man
in
had
as
y
surondig
ectra.
4751
w
an
the
star
disco
obtained
J16320
in
Chat
materil
w
ectra
elmn
Cam,
sgB[e]
has
ectrum
driguez
a
of
ed
CI
a
excitaon
ed
to
&
e
w
observ
y
b
ations
sp
en
INTEGRAL
absor
IGR
y
with
,
observ
them,
X-ra
b
also
sp
with
lo
Filatre
y
thic
Subseqn
harcteis,
simlart
ma
Infraed
and
not
some
infraed.
hig
has
er,
near
c
oth
leading
coun
is
b
tha
ho
J0421+56,
the
in
unprecd
coresp
&
13
Ro-
nature
has
XM-Newton
b
observ
en
ation,
204a).
s
Pulsation
ha
GRAL
v
e
source.
also
b
IGR
almost
60
s,
en
detc
from
J16358
the
4726
second
a
displa
longest
few
ys
P
other
absor
pulsation
kno
ed
with
wn(
P
atel
INTE-
a
et
al.
p
erio
d
of
204).
In-
s
tersingly
,
transie
t,
its
authors
as
eld.
it
thes
it
As
is
lik
v
p
e
those
of
e
et
y
the
p
eculiar
it
w
fern
ev
t
c
er,
thes
v
e
en
b
b
e
tings
rathe
en
v
of
arible,
only
a
smal
conrmed
their
sp
vino
to
to
hard
v
are
new
of
this
kno
et
ectra
w
the
e
b
e
(204b)
This
ard
b
and
al.
MXBs.
source
wn
b
e
sem
Galcti
arms
ciated
the
ap
In
hea
terpas
vy
of
ear
for
unclear.
with
coun
not
excpt
is
aso
far,
do
MXBs,
absorptin
to
ther
are
reason
harcteis
to
from
the
source
tremly
short
the
displa
w
traion
of
of
sem
INTEGRAL
with
oin
to
the
the
higer
case
mas
of
los
most
of
IGR
from
its
thes
source
wn.
Ho
The
et
Luto
cone
those
So
unko
e
t
source
ertis
compani.
are
b
source,
vious
b
repsn
ha
y
INTEGRAL
from
orign
48,
to
p
to
source.
INTEGRAL
pro
t
The
J1638
ear
source
ob
oSAX
found
ed
ears
204b).
diern
absorptin.
newly
ap
Bep
ap
simlart
new
their
al.
princle,
extrmly
jects
absor
the
the
4726
eral
source
INTEGRAL
ed
of
b
v
ob
new
absor
vino
In
10
of
most
J16358
sev
new
on
conrmed
(Luto
other
the
other
tha
b
the
Based
suget
to
of
IGR
during
opulatin
of
pulsar.
tha
detc
the
the
far,
y
not
y
tha
of
So
as
man
ely
fraction
X-ra
w
found
(
<
1
IGR
d)
y
ed
b
eha
viour
p
eculiar
efor
of
of
as
203,
(Smith
ha
during
t
promtly
198).
e
dif-
wn.
w
o
iden
J1739
al.
v
kno
detc
XTE
et
source
previously
and
t
the
MXB
w
Augst
transie
b
some
3021
in
wn
simlar
tha
clase
J1739
outbrs
alredy-kno
think
thre
Recn
302,
tied
whic
h
t
ex-
Chandr
had
a
14
observ
ations
to
ha
XTE
v
e
J1739
sup
t
et
ards,
sort
y
et
coun
terpa
is
v
whic
certainly
h
a
b
as
optical
coun
turns
out
as
detc
to
the
terpa
b
of
out
t
b
an
OB
e
an
O8
Iaf
INTEGRAL
b
v
coun
an
a
204).
P
=
sup
t
IGR
single
candite
IGR
28
alez-
ergian
outbrs,
has
(Smith
(Gonz
OB
short
also
2619.
terpa
e
ery
204,
with
dis-
J1754
a
to
with
er
star
pulsation
y
IGR
detcion
turns
Septm
e
b
outbrs,
transie
in
could
ed
also
third
erd
MXBs,
w
w
h
A
disco
the
h
short
whic
205).
4507,
whic
source
alo
204),
al.
J1645
205),
extrmly
ations
al.
of
205).
second
of
observ
et
ticaon
al.
al.
a
same
XM-Newton
iden
(Smith
afterw
(Chat
the
et
the
Riestra
ed
(Negurla
Shortly
ying
w
302
ergian
pla
alo
s
ha
J1645
v
e
b
4507
en
disco
v
erd
s
in
XM-Newton
observ
sem
to
In
at
b
e
a
least
tha
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to
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y
t,
w,
the
implcatons
ther
has
ect
t
are
man
y
opulatin
b
they
ob
ha
ery
b
kno
wn
to
turn
v
e
of
source
could
v
distance
jects
new
e
can
at
of
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widespra
not
source,
sample
.
p
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could
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en
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ely
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e
toal
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near
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exp
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the
disco
in
v
kno
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terpas,
of
ob
the
is
a
Spanish
alo
resac
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MCyT
sup
b
sev
eral
new
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cirles
furthe
and
orted
b
y
the
the
the
in
smal
c
ohm
for
helpfu
progame
the
enough
for
harcteison
comen
R
Univ
ersit
Spanish
y
of
MCyT
I
en
er
ero
wing
of
ESP-2041C3.
Kreyk
v
vide
of
this
ts
author
partily
disco
pro
jects.
wledgmn
The
and
to
to
of
clas
Ac
y
INTEGRAL
XM-Newton
ery
tersing
b
ect
and
w
lik
ts
on
e
the
on
Alican
under
ould
am
te.
gran
to
thank
draft.
y
,
This
ts
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Cajl
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