Interplanetary Lyman-alpha spectra as a diagnostic of the local interstellar plasma density - The Baranov two-shocks heliosphere case

1992 ◽  
Vol 396 ◽  
pp. 696 ◽  
Author(s):  
R. Lallement ◽  
Iu. G. Malama ◽  
E. Quemerais ◽  
J. L. Bertaux ◽  
N. A. Zaitsev
Keyword(s):  
Plasma Density ◽  
Lyman Alpha ◽  
Interstellar Plasma

Design of a Lyman-Alpha-Based BES for edge plasma density diagnosing on the HL-2A tokamak

2021 ◽  
Vol 172 ◽  
pp. 112911
Author(s):  
Y.X. Zhou ◽  
Y. Yu ◽  
R. Ke ◽  
W. Jiang ◽  
M. Xu ◽  
...  
Keyword(s):  
Plasma Density ◽  
Edge Plasma ◽  
Lyman Alpha

scholarly journals A Lyman-alpha-based (VUV) plasma density fluctuation diagnostic design

2001 ◽  
Vol 72 (1) ◽  
pp. 992-995 ◽  
Author(s):  
G. R. McKee ◽  
R. J. Fonck ◽  
C. Fenzi ◽  
B. P. Leslie
Keyword(s):  
Plasma Density ◽  
Density Fluctuation ◽  
Lyman Alpha

Lyman-alpha as an Astrophysical and Cosmological Tool

2019 ◽  
Author(s):  
Mark Dijkstra ◽  
J. Xavier Prochaska ◽  
Masami Ouchi ◽  
Matthew Hayes
Keyword(s):  
Lyman Alpha

Ionized gas kinematics and luminosity profiles of Low-z Lyman Alpha Blobs

2019 ◽  
Vol 15 (S359) ◽  
pp. 413-414
Author(s):  
María P. Agüero ◽  
Rubén Díaz ◽  
Mischa Schirmer
Keyword(s):  
Emission Line ◽  
Galactic Nuclei ◽  
Host Galaxies ◽  
Ionized Gas ◽  
Lyman Alpha ◽  
Gas Kinematics ◽  
The Universe ◽  
Very High ◽  
The Continuum

AbstractThis work is focused on the characterization of the Seyfert-2 galaxies hosting very large, ultra-luminous narrow-line regions (NLRs) at redshifts z = 0.2−0.34. With a space density of 4.4 Gcp−3 at z ∼ 0.3, these “Low Redshift Lyman-α Blob” (LAB) host galaxies are amongst the rarest objects in the universe, and represent an exceptional and short-lived phenomenon in the life cycle of active galactic nuclei (AGNs). We present the study of GMOS spectra for 13 LAB galaxies covering the rest frame spectral range 3700–6700 Å. Predominantly, the [OIII]λ5007 emission line radial distribution is as widespread as that of the continuum one. The emission line profiles exhibit FWHM between 300–700 Km s−1. In 7 of 13 cases a broad kinematical component is detected with FWHM within the range 600–1100 Km s−1. The exceptionally high [OIII]λ5007 luminosity is responsible for very high equivalent width reaching 1500 Å at the nucleus.

scholarly journals Solar Irradiance Variability Due to Solar Flares Observed in Lyman-Alpha Emission

Solar Physics ◽  
2021 ◽  
Vol 296 (3) ◽  
Author(s):  
Ryan O. Milligan
Keyword(s):  
Solar Flares ◽  
Solar Spectrum ◽  
Neutral Hydrogen ◽  
Solar Limb ◽  
High Background ◽  
Superposed Epoch Analysis ◽  
Lyman Alpha ◽  
Alpha Emission ◽  
Epoch Analysis ◽  
Very High

AbstractAs the Lyman-alpha (Ly$\upalpha $ α ) line of neutral hydrogen is the brightest emission line in the solar spectrum, detecting increases in irradiance due to solar flares at this wavelength can be challenging due to the very high background. Previous studies that have focused on the largest flares have shown that even these extreme cases generate enhancements in Ly$\upalpha $ α of only a few percent above the background. In this study, a superposed-epoch analysis was performed on ≈8500 flares greater than B1 class to determine the contribution that they make to changes in the solar EUV irradiance. Using the peak of the 1 – 8 Å X-ray emission as a fiducial time, the corresponding time series of 3123 B- and 4972 C-class flares observed in Ly$\upalpha $ α emission by the EUV Sensor on the Geostationary Operational Environmental Satellite 15 (GOES-15) were averaged to reduce background fluctuations and improve the flare signal. The summation of these weaker events showed that they produced a 0.1 – 0.3% enhancement to the solar Ly$\upalpha $ α irradiance on average. For comparison, the same technique was applied to 453 M- and 31 X-class flares, which resulted in a 1 – 4% increase in Ly$\upalpha $ α emission. Flares were also averaged with respect to their heliographic angle to investigate any potential center-to-limb variation. For each GOES class, the relative enhancement in Ly$\upalpha $ α at the flare peak was found to diminish for flares that occurred closer to the solar limb due to the opacity of the line and/or foreshortening of the footpoints. One modest event included in the study, a C6.6 flare, exhibited an unusually high increase in Ly$\upalpha $ α of 7% that may have been attributed to a failed filament eruption. Increases of this magnitude have hitherto only been associated with a small number of X-class flares.

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