Catching Some Sun: Probing the Solar Wind with Cometary X-Ray and Far-Ultraviolet Emission

2004 ◽  
Vol 606 (1) ◽  
pp. L81-L84 ◽  
Author(s):  
D. Bodewits ◽  
Z. Juhsz ◽  
R. Hoekstra ◽  
A. G. G. M. Tielens
Keyword(s):  
Solar Wind ◽  
Ultraviolet Emission ◽  
X Ray ◽  
Far Ultraviolet

PROBING THE SOLAR WIND WITH COMETARY X-RAY AND FAR-ULTRAVIOLET EMISSION

2006 ◽  
Author(s):  
R. HOEKSTRA ◽  
D. BODEWITS ◽  
R. MORGENSTERN ◽  
C. M. LISSE ◽  
A. G. G. M. TIELENS
Keyword(s):  
Solar Wind ◽  
Ultraviolet Emission ◽  
X Ray ◽  
Far Ultraviolet

scholarly journals Winds from Cool Stars

2004 ◽  
Vol 219 ◽  
pp. 623-634 ◽  
Author(s):  
A. K. Dupree
Keyword(s):  
Solar Wind ◽  
Infrared Observations ◽  
X Ray ◽  
Cool Stars ◽  
Comprehensive Picture ◽  
Far Ultraviolet

Recent spectroscopic results from the far ultraviolet and X-ray region coupled with infrared observations demonstrate that winds from luminous stars can be warm (300000K) and fast (speeds of several hundred km s—1) linking the hot solar wind to the cool, massive winds of luminous M-type supergiant stars. Hot coronal material (T ∼107 K) appears to be confined near the star, and not expanding in the wind. These new spectra enable a comprehensive picture to be constructed of the presence and character of winds in cool stars.

scholarly journals The impact of stellar activity on planets

2006 ◽  
Vol 2 (14) ◽  
pp. 295-296
Author(s):  
Ignasi Ribas
Keyword(s):  
Solar Wind ◽  
Solar System ◽  
Stellar Activity ◽  
Particle Emissions ◽  
X Ray ◽  
The Past ◽  
Far Ultraviolet ◽  
The Impact

AbstractThe results of the Sun in Time program indicate that the X ray, far ultraviolet and ultraviolet fluxes of the young Sun were significantly higher than today. Similarly, the solar wind mayhave been much stronger in the past. Such environment of intense energy and particle emissions could have influenced the paleo-atmospheres of Solar System planets and, by extension, the habitability and stability of exoplanets.

X-Ray and Far-Ultraviolet Emission from Comets: Relevant Charge Exchange Processes

2004 ◽  
Vol 70 (6) ◽  
pp. C17-C20 ◽  
Author(s):  
D Bodewits ◽  
R W McCullough ◽  
A G G M Tielens ◽  
R Hoekstra
Keyword(s):  
Charge Exchange ◽  
Ultraviolet Emission ◽  
X Ray ◽  
Exchange Processes ◽  
Far Ultraviolet

A Calculation real abundance of gaseous elements of the comet PanSTARRS C/2011 S4

2020 ◽  
Vol 18 (45) ◽  
pp. 21-31
Author(s):  
Salman Zaidan Khalaf ◽  
Khaleel Abrahim ◽  
Imad Kassar Akeab
Keyword(s):  
Solar Wind ◽  
Physical Properties ◽  
Atomic Number ◽  
Mathematic Model ◽  
Emission Energy ◽  
X Ray ◽  
The Real

    X-ray emission contains some of the gaseous properties is produced when the particles of the solar wind strike the atmosphere of comet ISON and PanSTARRS Comets. The data collected with NASA Chandra X-ray Observatory of the two comets, C/2012 S1 (also known as Comet ISON) and C/2011 S4 (Comet PanSTARRS) are used in this study.    The real abundance of the observed X-ray spectrum elements has been extracted by a new simple mathematic model. The study found some physical properties of these elements in the comet’s gas such as a relationship between the abundance with emitted energy. The elements that have emission energy (2500-6800) eV, have abundance (0.1-0.15) %, while the elements that have emission energy (850-2500) eV and (6800-9250) eV have abundance (0.2-0.3) %.    The relation between interacted energy and atomic number is form two sets.  The interacted energy of each element is increased as the atomic number increased. This case has been seen in both comets

High-resolution far ultraviolet emission spectra of electron-excited molecular deuterium

1999 ◽  
Vol 32 (15) ◽  
pp. 3813-3838 ◽  
Author(s):  
H Abgrall ◽  
E Roueff ◽  
Xianming Liu ◽  
D E Shemansky ◽  
G K James
Keyword(s):  
High Resolution ◽  
Emission Spectra ◽  
Ultraviolet Emission ◽  
Far Ultraviolet

Synthesis and Luminescence Properties of Chalcopyrite-Type CuAlS2

2006 ◽  
Vol 301 ◽  
pp. 177-180 ◽  
Author(s):  
Yuichiro Kuroki ◽  
Tomoichiro Okamoto ◽  
Masasuke Takata
Keyword(s):  
Diffraction Analysis ◽  
Room Temperature ◽  
Single Phase ◽  
Elevated Temperatures ◽  
Emission Peak ◽  
Maximum Intensity ◽  
X Ray Diffraction ◽  
Ultraviolet Emission ◽  
X Ray ◽  
Copper Aluminum

Copper aluminum disulfide (CuAlS2) powders were synthesized in an evacuated ampoule at elevated temperatures. X-ray diffraction analysis revealed that the powders heated at temperatures higher than 800oC were single-phase CuAlS2. In the cathodoluminescence (CL) spectra measured at room temperature, the powders heated at temperatures higher than 600oC exhibited a visible emission peak at approximately 1.8 eV and a distinct ultraviolet emission peak at 3.45 eV. The powder heated at 700oC showed the maximum intensity of ultraviolet emission which is considered to be associated with excitons.

Structure and strong ultraviolet emission characteristics of amorphous ZnO films grown by electrophoretic deposition

2003 ◽  
Vol 18 (1) ◽  
pp. 151-155 ◽  
Author(s):  
Zhijian Wang ◽  
Haiming Zhang ◽  
Zhijun Wang ◽  
Ligong Zhang ◽  
Jinshan Yuan ◽  
...  
Keyword(s):  
Electrophoretic Deposition ◽  
Indium Tin Oxide ◽  
Zno Films ◽  
Emission Characteristics ◽  
Photoluminescence Intensity ◽  
Ultraviolet Emission ◽  
X Ray ◽  
Glass Substrates ◽  
Strong Ultraviolet Emission ◽  
Zno Powder

Structure and ultraviolet emission characteristics of amorphous ZnO films grown on indium tin oxide coated glass substrates by electrophoretic deposition were investigated using Raman spectra and photoluminescence. The Raman spectrum shows a unique resonant multiphonon process within amorphous ZnO films. The photoluminescence spectrum of amorphous ZnO films shows a strong ultraviolet emission while the visible emission is nearly fully quenched. The transmission electron microscopy, x-ray diffraction, x-ray photoelectron spectrum, and infrared spectrum are used to detect the structure of amorphous ZnO powder. The complex water plays an important role in the photoluminescence intensity emission.

MHD simulations of magnetospheric response to a strong solar wind density pulse

2021 ◽  
Author(s):  
Andrey Samsonov ◽  
Jennifer A. Carter ◽  
Graziella Branduardi-Raymont ◽  
Steven Sembay
Keyword(s):  
Solar Wind ◽  
Dynamic Pressure ◽  
Solar Wind Density ◽  
Ionospheric Currents ◽  
X Ray ◽  
Interplanetary Coronal Mass Ejection ◽  
Explorer Mission ◽  
The One ◽  
Mass Ejection ◽  
Present Simulation

<p>On 16-17 June 2012, an interplanetary coronal mass ejection with an extremely high solar wind density (~100 cm<sup>-3</sup>) and mostly strong northward (or eastward) interplanetary magnetic field (IMF) interacted with the Earth’s magnetosphere. We have simulated this event using global MHD models. We study the magnetospheric response to two solar wind discontinuities. The first is characterized by a fast drop of the solar wind dynamic pressure resulting in rapid magnetospheric expansion. The second is a northward IMF turning which causes reconfiguration of the magnetospheric-ionospheric currents. We discuss variations of the magnetopause position and locations of the magnetopause reconnection in response to the solar wind variations. In the second part of our presentation, we present simulation results for the forthcoming SMILE (Solar wind Magnetosphere Ionosphere Link Explorer) mission. SMILE is scheduled for launch in 2024. We produce two-dimensional images that derive from the MHD results of the expected X-ray emission as observed by the SMILE Soft X-ray Imager (SXI). We discuss how SMILE observations may help to study events like the one presented in this work.</p>

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