PN | MOS | RGS | |
Abundancesa, b (
![]() |
|||
C | =Fe | =Fe |
![]() |
N | =Fe | =Fe |
![]() |
O |
![]() |
![]() |
![]() |
Ne |
![]() |
![]() |
![]() |
Mg |
![]() |
![]() |
![]() |
Si |
![]() |
![]() |
=Fe |
S |
![]() |
![]() |
=Fe |
Fe |
![]() |
![]() |
0.1 |
Ni |
![]() |
![]() |
=![]() |
Temperatureb (K) | |||
![]() |
![]() |
![]() |
|
![]() |
![]() |
![]() |
|
![]() |
![]() |
![]() |
|
Emission measureb
![]() |
|||
![]() |
![]() |
![]() |
|
![]() |
![]() |
![]() |
|
![]() |
![]() |
![]() |
|
Column densityb (
![]() |
|||
![]() |
![]() |
![]() |
=1 |
Best fit statistics | |||
![]() |
0.89 | 0.99 | |
d.o.f. | 404 | 285 | |
![]() |
94% | 54% |
a Solar photospheric abundances are from Anders & Grevesse (1989). b All the uncertainties correspond to the 68% confidence level. |