scholarly journals Magnetohydrodynamics of Mira’s cometary tail

2013 ◽  
Vol 558 ◽  
pp. A107 ◽  
Author(s):  
E. A. Gómez
Keyword(s):  
Cometary Tail

scholarly journals On the size of the cometary tail magnetic field

1979 ◽  
Vol 188 (4) ◽  
pp. 727-733 ◽  
Author(s):  
D. A. Mendis ◽  
P. J. Morrison
Keyword(s):  
Magnetic Field ◽  
Cometary Tail

scholarly journals Physical Processes in Cometary Atmospheres

1972 ◽  
Vol 45 ◽  
pp. 253-259 ◽  
Author(s):  
A. Z. Dolginov
Keyword(s):  
Rotation Period ◽  
Dust Particles ◽  
Molecular Flow ◽  
Physical Parameters ◽  
Charged Dust ◽  
Nuclear Surface ◽  
Cometary Dust ◽  
Meteor Streams ◽  
Cometary Tail ◽  
Dust Component

Formulae are obtained for the distribution of molecules in the cometary head, taking into account the conditions of hydrodynamic and free molecular flow in various regions around the nucleus. Experimental data are used to derive physical parameters near the nuclei of comets 1952 III, 1955 V, 1957 III, and 1960 II and the rate of decrease of mass. The possibility of chemical reactions in the region close to the nucleus is discussed. Gas condensation is shown to be a possible cause of dust formation under the conditions existing near the nucleus, and this process may be responsible for the major portion of the cometary dust component. The observed grouping of synchrones in the cometary tail can be explained on the assumption that the nuclear surface comprises two (or more) areas differing essentially in evaporation rate, the amount of matter ejected varying over the rotation period of the nucleus. Charged dust particles are shown to form, with electrons and ions, a common medium, i.e., dust plasma, which can be treated by the same methods used for ordinary plasma. Special investigations appear to be desirable when comets intersect meteor streams.

scholarly journals Sh 2-68 – A Planetary Nebula Leaving it's Mark on the Interstellar Medium

2003 ◽  
Vol 209 ◽  
pp. 525-526 ◽  
Author(s):  
F. Kerber ◽  
F. Guglielmetti ◽  
R. Mignani ◽  
M. Roth
Keyword(s):  
Interstellar Medium ◽  
Planetary Nebula ◽  
Galactic Disk ◽  
Central Star ◽  
Main Body ◽  
Left Behind ◽  
Sky Survey ◽  
Cometary Tail ◽  
Direct Confirmation

Using Hα images from the Southern H-Alpha Sky Survey Atlas (SHASSA) we have discovered a “cometary tail” of ionized matter extending at least 30 arcmin from the main body of the planetary nebula Sh 2-68 (PN G030.6+06.2). This tail is aligned with the proper motion of the central star and is obviously a contrail of material left behind by Sh 2-68 moving in a Galactic Disk orbit. The tail's existence is a direct confirmation of Sh 2-68's interaction with the interstellar medium (ISM) and highlights the possibly important role of the ISM's magnetic field.

An argument against a type I cometary tail model

1975 ◽  
Vol 32 (2) ◽  
pp. L19-L23 ◽  
Author(s):  
Karl Wurm
Keyword(s):  
Type I ◽  
Cometary Tail

scholarly journals A global model of cometary tail disconnection events triggered by solar wind magnetic variations

2007 ◽  
Vol 112 (A5) ◽  
pp. n/a-n/a ◽  
Author(s):  
Ying-Dong Jia ◽  
Michael R. Combi ◽  
Kenneth C. Hansen ◽  
Tamas I. Gombosi
Keyword(s):  
Solar Wind ◽  
Global Model ◽  
Cometary Tail

Terrestrial cometary tail and lunar corona induced by small comets: Predictions for Galileo

1990 ◽  
Vol 17 (12) ◽  
pp. 2257-2260 ◽  
Author(s):  
A. J. Dessler ◽  
B. R. Sandel ◽  
V. M. Vasyliunas
Keyword(s):  
Cometary Tail

scholarly journals A Kinematographic Study of the Tail of Comet Kohoutek (1973f)

1976 ◽  
Vol 25 (Part1) ◽  
pp. 370-377 ◽  
Author(s):  
K. Jockers ◽  
R. G. Roosen ◽  
D. P. Cruikshank
Keyword(s):  
High Speed ◽  
Plasma Tail ◽  
Flat Field ◽  
Cometary Tail ◽  
Made In

By combining observations of Comet Kohoutek (1973 f) made in the Southwest US, Alaska and Hawaii, a cometary tail movie has been made. Parts of the movie were shown at the conference and some frames of the movie are reproduced in Fig. 1, In this paper we give some details of the observations and describe what we see on the movie.Observers who contributed to the movie are listed in Table 1 with their institutions, instruments, and site locations. In all but one case, fast Schmidt cameras were used; high-speed optics are needed for this work because the interval between successive pictures should not exceed 15 minutes if plasma tail motions are to be properly visualized. The 36 cm f/2 Schmidt camera of the Joint Observatory for Cometary Research (JOCR) is clearly well-suited because of its flat field of about 8 x 10°.

scholarly journals Effects of radiation pressure on the evaporative wind of HD 209458b

2020 ◽  
Vol 493 (1) ◽  
pp. 1292-1305 ◽  
Author(s):  
Alex Debrecht ◽  
Jonathan Carroll-Nellenback ◽  
Adam Frank ◽  
Eric G Blackman ◽  
Luca Fossati ◽  
...  
Keyword(s):  
Radiation Pressure ◽  
High Energy ◽  
Line Of Sight ◽  
Hydrodynamic Simulation ◽  
High Energy Radiation ◽  
Hydrodynamic Simulations ◽  
Cometary Tail ◽  
Effects Of Radiation ◽  
Simplified Calculation

ABSTRACT The role of radiation pressure in shaping exoplanet photoevaporation remains a topic of contention. Radiation pressure from the exoplanet’s host star has been proposed as a mechanism to drive the escaping atmosphere into a ‘cometary’ tail and explain the high velocities observed in systems where mass-loss is occurring. In this paper, we present results from high-resolution 3D hydrodynamic simulations of a planet similar to HD 209458b. We self-consistently launch a wind flowing outwards from the planet by calculating the ionization and heating resulting from incident high-energy radiation, and account for radiation pressure. We first present a simplified calculation, setting a limit on the Lyman-α flux required to drive the photoevaporated planetary material to larger radii and line-of-sight velocities. We then present the results of our simulations, which confirm the limits determined by our analytic calculation. We thus demonstrate that, within the limits of our hydrodynamic simulation and for the Lyman-α fluxes expected for HD 209458, radiation pressure is unlikely to significantly affect photoevaporative winds or to explain the high velocities at which wind material is observed, though further possibilities remain to be investigated.

Near-tail reconnection as the cause of cometary tail disconnections

1986 ◽  
Vol 91 (A2) ◽  
pp. 1417 ◽  
Author(s):  
C. T. Russell ◽  
M. A. Saunders ◽  
J. L. Phillips ◽  
J. A. Fedder
Keyword(s):  
Cometary Tail
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