The escape occurs mostly above a certain level in the upper atmosphere known as Exobase where the transition from collision gas occurs to collision gas (Figure 10). Below Exobase, the atmosphere can be dealt with as liquid, because the average distance that the molecule or corn travels before a collision – the medium free path – is shorter than the smallest sample length scale. The latter is usually defined by the height of the H, which distinguishes the ingredient of the pressure of the pressure with the height.
Above exobase is an unprecedented area known as Exosphere, where the medium free path exceeds the height of the atmosphere. Sufficiently sufficient collision because atoms and neutral particles carry out dynamic paths that are often affected by the IO and Jupiter field.
Exobase is defined to the state of hydrostatic balance, in addition to one species represented at a single temperature. The definition similar to the corresponding height in a dynamic column with loose flow speed is not possible. McDwell and others. (2017) It has shown that high -pillar particles above Exobase for a purely published atmosphere may be bounced off the permitted atmosphere near Exobase when retreating to the surface (Figure 11, right). In large columns, it is possible that the level in which the quick particles can escape sufficiently without collision of umbrella shock, which is expected to be higher than the Exobase in the Summers and Strobel, 1996; McDoniel et al., 2017).
We also note that the upper part of IO’s atmosphere is not in the local thermal dynamic balance (LTE) and thus may have different categories of molecules or atoms different temperatures and thus Exobase rises.
In general, the ejaculation pillar gases do not contain enough speeds to escape the risk of IO directly. Under the ballistic conditions (without collision), to reach a height of 400 km as it was deduced to the highest columns, a 1.2 km/s expelling speed is needed. This is still much lower than the IO Escape speed of 2.56 km/s or speed to reach the radius of the diameter of the hill (half of the diameter where the IO appeal is equal to Jupiter, near 5.8 Rio) from 2.33 km/s. Assuming the MaxWellian speed distribution with a high temperature of 800 K about a large upward speed of 1.2 km/s, only less than 10-5 of SO2 SIM particles up to escape speed. Even with the extensive SO2 gas source rate of 105 kg/s, this results in an escape rate of 1 kg/s, which is three orders less than the ecclesiastical number. The speed of the expulsion, gas temperatures and SO2 source rates that are usually assumed to simulate large columns such as the Pele column are less than our assumptions here (Zhang et al., 2003; 2004; McDoniel et al In addition, simulation operations revealed that the ejaculation pillar gas is actually slowing through the decrease in gases in the umbrella shocks, which increases the increase in fracture (Zhang et al., 2003).
This position differs greatly from the Ecsellados column, where the surface gravity is 6 % of IO’s surface gravity and the part of the fugitive molecules is higher than those higher than those who return to the surface (for example, Tian et al., 2007; Villanueva et al., 2023). However, we note that there may be possible paths for direct volcanic escape that has not yet been explored, such as the dynamic behavior of developments that arise from hot surface lava with 1200 km or higher temperatures.
In an atmosphere linked to the form of gravity with Exosphere, the main non -dimensional parameter that governs escape is the jeans λ, which is defined as being
Authors:
(1) L. Roth, KTH ROYAL Institute of Technology, Space and Plasma Physics, Stockholm, Sweden and the opposite author;
(2) A. Bloker, Cole Royal Institute of Technology, Space Physics and Plasma, Stockholm, Sweden and Earth and Environmental Sciences Department, University of Ludwig Maximilian in Munich, Munich, Germany;
(3) K.
(4) d. Goldstein, Department of Engineering and Engineering, University of Texas in Austin, Austin, Texas, USA;
(5) E. Lellouch, Laboratoire D’ETudes Spatials et d’Artarch en asrophysique (Lesia), obsefatoire de Paris, Meudon, France;
(6) J
(7) C. Schmidt, Space Physics Center, Boston University, Boston, Massachusetts, USA;
(8) DF Strobel, Department of Science, Physics and Astronomy, Jones Hopkins University, Baltimore, MD 21218, USA;
(9) C. TAO, National Institute of Information and Communications Technology, Koganei, Japan;
(10) F. Tsuchia, College of Graduate Studies for Science, University of Tuoku, Sendai, Japan;
(11) V. DOLS, Institute of Astronomical Physics and Planetary Science, National Institute of Astronomical Physics, Italy;
(12) H
(13) a. Mora, xx;
(14) JR Szalay, Department of Astronomical Physical Sciences, Princeton University, Princeton, New Jersey, USA;
(15) SV Badman, Department of Physics, University of Lancaster, Lancaster, La1 4YB, UK;
(16) E.
(17) A.-C. Dott, Geophysics and Meteorological Institute, Colonia University, Cologne, Germany;
(18) M. Kajaitani, College of Graduate Studies for Science, University of Tuoku, Sendai, Japan;
(19) L. Klaiber, Institute of Physics, University of Bern, 3012 Bern, Switzerland;
(20) R. Koga, Department of Earth Sciences and Planets, University of Nagoya, Nagoya, Ishi 464-8601, Japan;
(21) A. MCEWEN, Department of Astronomy, Earth Sciences and Planets Department, University of California, Berkeley, California 94720, USA;
(22) Z. Milby, Department of Geological Sciences and Planets, California Institute of Technology, Pasadina, California 91125, USA;
(23) Kd Retherford, South Western Research Institute, San Antonio, Texas, USA and Texas University in San Antonio, San Antonio, Texas, USA;
(24) S. Schlegel, Geophysics and Meteorological Institute, University of Cologne, Cologne, Germany;
(25) N. Thomas, Institute of Physics, Bern University, 3012 Bern, Switzerland;
(26) WL TSING, Department of Earth Sciences, Taiwan National University, Taiwan;
(27) a. Foreberger, Institute of Physics, Bern University, 3012 Bern, Switzerland.
