X-rays from solar system objects

Preface Part I Setting the stage Part 2 Magnetic fields Part 3 Magnetospheric accretion and inner disk truncation Part 4 Magnetospheric ejection Part 5 Star-disk magnetospheric coupling Part 6 Companions, planets and effects of stellar mass Part 7 Conclusion Author index subject index Object Index

Star-disk interaction in young stars : proceedings of the 243th symposium of the International Astronomical Union held in Grenoble, France, May 21-25, 2007

Solar wind charge-exchange (SWCX) emission is present in every X-ray observation of an astrophysical object. The emission is problematic when one cannot remove the foreground by the simultaneous measurement of a nearby field. SWCX emission is a serious impediment to the study of the diffuse hot ISM, including the galactic halo, as its contribution to diagnostic emission lines is temporally variable. Modeling the SWCX emission, in order to remove it from our observations, has proven to be more difficult than originally anticipated. This work reviews our current understanding of SWCX emission, with special attention to all the components required for future modeling tools. Since, in the absence of such a tool, observing programs can still be constructed to minimize the effect of SWCX, mitigation strategies are discussed. Although some aspects of SWCX will be very difficult to characterize, progress continues on many fronts.

Solar wind charge exchange: an astrophysical nuisance

The work presents modern ideas on the physical mechanism of explosion of large meteoroids (superbolides) in the Earth’s atmosphere at the end of their trajectories. As a result of our work, the values of following parameters were obtained: the altitude of the beginning of the aerodynamic destruction of a meteoroid like the Chelyabinsk superbolide; the altitude of a relatively very thin layer, characterized by sharp aerodynamic deceleration of a fragmenting and laterally expanding space object, accompanied by an impulse transformation of kinetic energy into thermal energy with plasma generation which results in intense electromagnetic radiation and an explosive shock wave; and, the initial temperature of such a plasma.

Physical mechanism of Chelyabinsk superbolide explosion

Observation results are presented for the lower and upper ionosphere disturbances accompanying the passage and explosion of the Chelyabinsk space body. The effects near the meteoroid’s path are investigated from the total electron content variations detected by GPS radio receivers. The ionosphere observations at distances of ∼2000-300 km are based on the ionosonde data and the phase and amplitude measurements for a radio signal at 66.67 kHz on the route from Moscow to Kharkiv. Manifestations are found both of acoustic and gravity waves following the passage and explosion of the space body. Their connection with the passage of the Chelyabinsk meteoroid is discussed.

Ionospheric effects of the Chelyabinsk meteoroid

Abstract It is analytically shown that passages of comets near the Sun's surface with velocities more than 600 km/s is accompanied by aerodynamic crushing of their nuclei within the solar chromosphere and transversal expansion of the crushed matter. The deceleration of the flattened hypervelocity body within the solar photosphere has sharply impulsive and strongly explosive character. The specific energy release in the explosion zone near the solar surface 10-100 thousand times exceeds the evaporation heat of the nucleus material, so that the process is accompanied by generation of high-temperature plasma and non-stationary explosive phenomena around the photosphere. Spectral observations of these phenomena by SOHO and SDO type space observatories with high spatial and temporal resolutions are of interest for the plasma astrophysics as well as the physics of solar flares.

/pdf/solar-plasma-generated-by-sungrazing-comets-1r1ctamuxb.pdf

Solar plasma generated by sungrazing comets

Abstract Explosive evolution of nuclei of sungrazing comets near the solar surface, which occurs at conditions of intense interaction between the solar atmosphere and falling high-velocity comet nuclei as well as the relation of the phenomenon to the character of solar activity are analytically considered. It is found that, due to aerodynamic fragmentation of the falling body in the solar chromosphere and transversal expansion of the fragmented mass under the action of pressure gradient on the frontal surface, thermalization of the kinetic energy of the body occurs by sharp stopping of the disklike hypervelocity fragmented mass near the solar surface within a relatively very thin subphotospheric layer and has, therefore, an essentially impulsive and strongly explosive character. The specific energy release in the explosion region, erg/g, considerably exceeds the evaporation/sublimation heat of the body so that the process is accompanied by production of a high-temperature plasma. The energetics of such an explosive process corresponds to that of very large solar flares for falling bodies having masses equal to the mass of the nucleus of Comet Halley. Spectral observations of sungrazing comets by SOHO-like telescopes in a wide spectral range, including X rays, with a high time resolution, of the order of 0.1–10 s, are important for revealing solar activity in the form of an impact-generated photospheric flare.

/pdf/explosion-of-sungrazing-comets-in-the-solar-atmosphere-and-71ylfw6uq0.pdf

Explosion of sungrazing comets in the solar atmosphere and solar flares

Interplanetary dust interaction with comets: Production of x-rays

The intensity of solar X-radiation scattered by a comet is calculated and compared to the proper X-radiation of the comet due to impacts of cometary and interplanetary dust particles. Detection of X-radiation of dusty comets at small heliocentric distances (R ≤ 1 a. u.) is found to be an indicator of high-temperature plasma generation as result of grain collisions.

On Two Mechanisms of X-Ray Generation in Comets

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