An ionization gradient across the front in M17 SW

1983 ◽  
Vol 275 ◽  
pp. 130
Author(s):  
D. F. Lester ◽  
H. L. Dinerstein ◽  
D. M. Rank ◽  
D. H. Wooden
Keyword(s):  
Ionization Gradient

Methodologies for determination of soil ionization gradient

2012 ◽  
Vol 70 (5) ◽  
pp. 457-461 ◽  
Author(s):  
Fani E. Asimakopoulou ◽  
Ioannis F. Gonos ◽  
Ioannis A. Stathopulos
Keyword(s):  
Soil Ionization ◽  
Ionization Gradient

scholarly journals A detailed study on the reflection component for the black hole candidate MAXI J1836−194

2020 ◽  
Vol 493 (2) ◽  
pp. 2178-2187
Author(s):  
Yanting Dong ◽  
Javier A García ◽  
Zhu Liu ◽  
Xueshan Zhao ◽  
Xueying Zheng ◽  
...  
Keyword(s):  
Black Hole ◽  
Spectral Analysis ◽  
Primary Source ◽  
Ionization State ◽  
X Ray ◽  
Black Hole Candidate ◽  
Reflection Model ◽  
Iron Abundance ◽  
Reflection Component ◽  
Ionization Gradient

ABSTRACT We present a detailed spectral analysis of the black hole candidate MAXI J1836−194. The source was caught in the intermediate state during its 2011 outburst by Suzaku and RXTE. We jointly fit the X-ray data from these two missions using the relxill model to study the reflection component, and a steep inner emissivity profile indicating a compact corona as the primary source is required in order to achieve a good fit. In addition, a reflection model with a lamp-post configuration (relxilllp), which is normally invoked to explain the steep emissivity profile, gives a worse fit and is excluded at 99 per cent confidence level compared to relxill. We also explore the effect of the ionization gradient on the emissivity profile by fitting the data with two relativistic reflection components, and it is found that the inner emissivity flattens. These results may indicate that the ionization state of the disc is not constant. All the models above require a supersolar iron abundance higher than ∼4.5. However, we find that the high-density version of reflionx can describe the same spectra even with solar iron abundance well. A moderate rotating black hole (a* = 0.84–0.94) is consistently obtained by our models, which is in agreement with previously reported values.

Quantitative Characteristics of Equatorial Ionization Gradient Above 150 km at Low Solar Activity

Radio Science ◽  
2018 ◽  
Vol 53 (8) ◽  
pp. 948-962 ◽  
Author(s):  
B. O. Adebesin ◽  
J. O. Adeniyi ◽  
O. A. Oladipo ◽  
A. O. Olawepo ◽  
I. A. Adimula
Keyword(s):  
Solar Activity ◽  
Quantitative Characteristics ◽  
Ionization Gradient

scholarly journals Narrowband HST images of microstructures in Planetary Nebulae

1997 ◽  
Vol 180 ◽  
pp. 208-208 ◽  
Author(s):  
B. Balick ◽  
J. Alexander ◽  
A. Hajian ◽  
Y. Terzian ◽  
M. Perinotto ◽  
...  
Keyword(s):  
Hubble Space Telescope ◽  
Planetary Nebulae ◽  
Space Telescope ◽  
Ionization Gradient

Hubble Space Telescope narrowband images of four PNe resolve the microstructures in four PNe known to contain FLIERs (e.g. Balick et al 1994). FLIERs are seen to fall into two morphological groups: very low ionization clumps of small knots with cometary-like tails, and sinewy transverse filaments with fainter extensions pointing outward from the nucleus. Generally speaking, FLIERs exhibit [NII]λ6584/Hα > 1. They are marginally detectable in Hα above the bright background of nebular emission, and all but invisible in [O III]λ5007A. In every case the star-facing side of the structure is on the order of a pixel in width (about 1015 cm). A decreasing ionization gradient is seen [O I]λ6300A, [S II]λ6717 + 31A, and [N II]λ6584A images.

Pattern of Ionization Gradient, Solar Quiet Magnetic Element, and F 2 ‐Layer Bottomside Thickness Parameter at African Equatorial Location

Radio Science ◽  
2019 ◽  
Vol 54 (5) ◽  
pp. 415-425
Author(s):  
B. O. Adebesin ◽  
J. O. Adeniyi ◽  
I. A. Adimula ◽  
S. J. Adebiyi ◽  
S. O. Ikubanni ◽  
...  
Keyword(s):  
Magnetic Element ◽  
Ionization Gradient ◽  
Thickness Parameter
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