148
A. Patruno and A. L. Watts
Table 4.1
(continued)
Source
ν
s
P
b
f
x
M
c,min
Companion type
Ref.
(Hz)
(h)
(M
)
(M
)
Symbiotic X-ray binaries
GX 1+4
6.3
× 10 −3
1161 days
M5 Giant
[66, 138, 274]
4U 1954+31
5.5
× 10 −5
M4 Giant
[64, 274]
IGR J16358-4724 b
1.7
× 10 −4
K/M Giant
[64, 274]
ν
s is the spin frequency, P
b the orbital period, f
x is the X-ray mass function, M
c,min is the minimum companion mass for an assumed NS mass of 1.4 M
.
The companion types are: WD
White Dwarf, BD
Brown Dwarf, MS
Main Sequence, SubG
Sub-Giant, He Core
Helium Star
a
The donor mass is inferred from photometric data and does represent the most likely mass
b
Binary with parameters that are still compatible with an intermediate/high mass donor
A. Patruno and A. L. Watts
Table 4.1
(continued)
Source
ν
s
P
b
f
x
M
c,min
Companion type
Ref.
(Hz)
(h)
(M
)
(M
)
Symbiotic X-ray binaries
GX 1+4
6.3
× 10 −3
1161 days
M5 Giant
[66, 138, 274]
4U 1954+31
5.5
× 10 −5
M4 Giant
[64, 274]
IGR J16358-4724 b
1.7
× 10 −4
K/M Giant
[64, 274]
ν
s is the spin frequency, P
b the orbital period, f
x is the X-ray mass function, M
c,min is the minimum companion mass for an assumed NS mass of 1.4 M
.
The companion types are: WD
White Dwarf, BD
Brown Dwarf, MS
Main Sequence, SubG
Sub-Giant, He Core
Helium Star
a
The donor mass is inferred from photometric data and does represent the most likely mass
b
Binary with parameters that are still compatible with an intermediate/high mass donor