X-Ray Emission from the Solar System Bodies: Connection with Solar X-Rays and Solar Wind

2010 ◽  
Author(s):  
Anil Bhardwaj ◽  
M. Maksimovic ◽  
K. Issautier ◽  
N. Meyer-Vernet ◽  
M. Moncuquet ◽  
...  
Keyword(s):  
Solar Wind ◽  
Solar System ◽  
X Rays ◽  
X Ray ◽  
Solar System Bodies

scholarly journals Simultaneous Observations of Large Enhancement In the Flux of PSR 0950+08 Over a 200 km Baseline at 103 MHz

1996 ◽  
Vol 160 ◽  
pp. 477-478
Author(s):  
A.D. Bobra ◽  
Harish Chandra ◽  
Hari Om Vats ◽  
P. Janardhan ◽  
G.D. Vyas ◽  
...  
Keyword(s):  
Solar Wind ◽  
Interplanetary Medium ◽  
Temporal Variations ◽  
X Rays ◽  
Physical Research Laboratory ◽  
X Ray ◽  
The Earth ◽  
Wind Velocities ◽  
Electro Magnetic ◽  
Galactic Radio

Interplanetary Scintillation (IPS) is a diffraction phenomenon in which coherent electro-magnetic radiation, from a distant radio source, passes through the solar wind, which is a turbulent refracting medium, and suffers scattering. This results in random temporal variations of the signal intensity (scintillation) at the Earth. IPS observations to monitor the interplanetary medium (IPM), to measure solar wind velocities in the directions of a number of compact extra-galactic radio sources and to estimate the angular diameters of their compact components have been carried out for many years at 103 MHz using the IPS facility (Alurkar et al. 1989) of the Physical Research Laboratory (PRL), Ahmedabad, India. Over a period of approximately 10 years of such observations, it has been seen that PSR 0950+08 has always remained well within the noise level. We observed a sudden enhancement in its flux (Deshpande et al. 1994) on 29 July, 1992. The ionospheric observations which are being carried out on a regular basis at PRL using an ionosonde also recorded a steep increase in the absorption index Fmin, which is an indicator of the excess ionization produced due to X-rays. During this period, the Sun was exceptionally quiet, thereby raising the question about the origin of the X-ray flux responsible for the observed steep rise in Fminduring the transit of PSR 0950+08.

Stellar-Mass Black Holes

2014 ◽  
Author(s):  
Charles D. Bailyn
Keyword(s):  
Black Holes ◽  
Solar System ◽  
Empirical Study ◽  
Stellar Mass ◽  
The Sun ◽  
X Rays ◽  
X Ray ◽  
New Class ◽  
Total Luminosity ◽  
The 1960S

This chapter examines stellar-mass black holes. The empirical study of black holes began in the 1960s with the discovery of quasars and the advent of X-ray astronomy. X-ray detectors could detect X-rays coming from a particular direction—as the instrument rotated, the detector scanned the sky. It was not expected that X-ray sources from outside the solar system would be detectable. However, it was quickly discovered that there were strong X-ray sources that appeared in the same position in every scan. The inferred luminosity of the sources was hundreds or thousands of times brighter than the Sun. When coincident optical stars were identified, they proved to be relatively faint. Thus, it was clear that a new class of celestial sources must exist whose radiation is predominantly in the form of X-rays, with a total luminosity comparable to or greater than that of ordinary stars.

scholarly journals On the development of a spherical hybrid model - Lessons and applications

2010 ◽  
Vol 6 (S274) ◽  
pp. 89-91
Author(s):  
S. Dyadechkin ◽  
E. Kallio ◽  
R. Jarvinen ◽  
P. Janhunen ◽  
V. S. Semenov ◽  
...  
Keyword(s):  
Solar Wind ◽  
Solar System ◽  
Hybrid Model ◽  
Preliminary Test ◽  
Status Report ◽  
New Model ◽  
Solar System Bodies

AbstractWe are developing a spherical hybrid model to study how the solar wind interacts with the solar system bodies. In this brief status report we introduce some lessons from the spherical grid development and illustrate the usage of the new model by showing a preliminary test run.

scholarly journals UkrVO Astroinformatics Software and Web-services

2016 ◽  
Vol 12 (S325) ◽  
pp. 361-366 ◽  
Author(s):  
I. B. Vavilova ◽  
Ya. S. Yatskiv ◽  
L. K. Pakuliak ◽  
I. L. Andronov ◽  
V. M. Andruk ◽  
...  
Keyword(s):  
Solar System ◽  
Web Services ◽  
Variable Stars ◽  
Virtual Observatory ◽  
X Ray ◽  
Orbital Parameters ◽  
The Public ◽  
Rotation System ◽  
The Earth ◽  
Solar System Bodies

AbstractThe aim of this paper is to introduce the software and astronomical web-services developed in frame of the Ukraine Virtual Observatory (UkrVO) and VIrtual Roentgen and Gamma Observatory (VIRGO) to the broad astronomical community. We report briefly on such web-services as the public databases “Sky Maps” of X-ray observations by XMM-Newton, the Earth Orbital Parameters for International Earth Rotation System, and the UkrVO Joint Digitized Archive of astroplates. We refer to such software as the “Multi-Column View”, “Variable Stars Calculator”, “FrameSmooth” for variable star’s research and “Collection Light Technology” (CoLiTec) software for search and discovery of new Solar System bodies.

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.

scholarly journals Charge-exchange soft x-ray emission of highly charged ions with inclusion of multiple-electron capture

2021 ◽  
Author(s):  
G Y Liang ◽  
X L Zhu ◽  
H G Wei ◽  
D W Yuan ◽  
J Y Zhong ◽  
...  
Keyword(s):  
Solar Wind ◽  
Electron Capture ◽  
Charge Exchange ◽  
Cross Sections ◽  
Line Intensity ◽  
X Rays ◽  
Double Electron Capture ◽  
X Ray ◽  
Double Electron ◽  
On Line

Abstract Charge-exchange has been recognized as a primary source of soft x-ray emission in many astrophysical outflow environments, including cometary and planetary exospheres impacted by solar wind. Some models have been setup by using different data collections of charge-exchange cross-sections. However, multiple electron transfer has not been included in these models. In this paper, we setup a charge exchange model with the inclusion of double-electron capture, and make a detailed investigation of this process on x-ray emissions of highly charged carbon, nitrogen, oxygen and neon ions by using available experimental cross-sections. We also study the effect of different n −selective cross-sections on soft x-ray emission by using available experimental n −distributions. This work reveals that double electron capture enhancement on line intensity is basically linearly proportional to the ratio of ion abundance in the solar wind. It is more obvious for soft x-rays from carbon ions (C4 +) in collision with CO2, and the enhancement on line intensity can be up to 53 per cent with typical ion abundances (ace observation) in solar wind. The synthetic spectra with parameters from the Ulysses mission for solar wind reveals velocity-dependence, target-dependence, as well as the non-negligible contribution from the double-electron capture.

scholarly journals X-ray emission from the solar wind

1970 ◽  
Vol 37 ◽  
pp. 408-412
Author(s):  
E. Boldt ◽  
A. Klimas ◽  
G. Sandri
Keyword(s):  
Solar Wind ◽  
Mean Free Path ◽  
Ecliptic Plane ◽  
Line Of Sight ◽  
Astronomical Unit ◽  
The Sun ◽  
X Rays ◽  
Electron Collisions ◽  
X Ray ◽  
Recent Developments

Recent developments have made it possible to detect cosmic X-rays with energies as low as several hundred eV. Several measurements of the diffuse X-radiation in this range have been reported (Baxter et al., 1969; Bowyer et al., 1968; Henry et al., 1968). In this note we investigate the possibility that these observers have detected X-radiation emitted by the solar wind. We conclude that they probably have not. However, we also find that bremsstrahlung may be detectable from a region of the sky near the sun. If this measurement is possible, it would represent an important method for determining some characteristics of the solar wind away from the ecliptic plane of the solar system. Even though the mean free path for electron collisions is large compared with the astronomical unit, the collision frequency, electron density, and energy released per encounter are sufficient to yield detectable soft X-radiation for lines of sight close to the sun. We have estimated the expected X-ray intensity in the vicinity of the earth on the basis of two models of the solar wind flow pattern; in the first, the flow is radial in all directions away from the sun, and in the second, the flow is confined to a disc of uniform thickness near the ecliptic. In both cases, we neglect temperature gradients for the electrons and compute the total flux received from interplanetary plasma along the line of sight. Most of the received intensity comes from the segment of the line of sight which is nearest the sun. The results are insensitive with respect to the position of the boundary of the solar cavity. Accordingly, we neglect the boundary and consider an infinitely large solar cavity.

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