Pub Date : 2024-08-01DOI: 10.1134/s0038094624700448
D. O. Amorim, T. V. Gudkova
Abstract
The Chandler wobble of Venus has been analyzed on the basis of the Earth-like models of the planet. The method for calculating the Chandler wobble period of Venus was tested on the example of the Earth. To take into account the inelasticity of the interior of a planet, the Andrade rheology was used; and the values of the rheologic model parameters, which can explain the observed period of the Chandler wobble of the Earth, were determined. Projections on the Chandler wobble period of Venus were obtained. For the most plausible models of the internal structure of Venus, in which the core radius is assumed to be within an interval of 3288 ± 167 km, the Chandler wobble period is 30–48 thousand years. A large error in the results is mainly caused by a wide range of probable values for the constant of precession of Venus.
{"title":"On the Chandler Period of Venus","authors":"D. O. Amorim, T. V. Gudkova","doi":"10.1134/s0038094624700448","DOIUrl":"https://doi.org/10.1134/s0038094624700448","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">Abstract</h3><p>The Chandler wobble of Venus has been analyzed on the basis of the Earth-like models of the planet. The method for calculating the Chandler wobble period of Venus was tested on the example of the Earth. To take into account the inelasticity of the interior of a planet, the Andrade rheology was used; and the values of the rheologic model parameters, which can explain the observed period of the Chandler wobble of the Earth, were determined. Projections on the Chandler wobble period of Venus were obtained. For the most plausible models of the internal structure of Venus, in which the core radius is assumed to be within an interval of 3288 ± 167 km, the Chandler wobble period is 30–48 thousand years. A large error in the results is mainly caused by a wide range of probable values for the constant of precession of Venus.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":null,"pages":null},"PeriodicalIF":0.9,"publicationDate":"2024-08-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141881283","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-08-01DOI: 10.1134/s0038094624700485
V. V. Svettsov
Abstract—
Semianalytical pancake models published in the literature are considered, in which it is assumed that a low-strength, fragmented body, like a liquid, expands during flight in the atmosphere and, while maintaining a certain simple shape and increasing the cross-sectional area, decelerates at much higher altitudes than a strong body. Individual models differ in the rate of increase in the transverse size of the body. For comparison with the models, hydrodynamic simulations of falls of liquid bodies with a diameter of 40 m in the Earth’s atmosphere were carried out without taking into account ablation. Such bodies, before they begin to slow down significantly, break up into fragments. Unlike simple models, while the body remains coherent, it can take on very distorted shapes. Comparison of pancake models with the results of hydrodynamic modeling allows us to determine the most suitable models for assessing the behavior of asteroids in the atmosphere and evaluate the assumptions embedded in them. In hydrodynamic modeling taking into account ablation, as shown by the results published in other works, complete evaporation of the body can first occur and, only then, the braking of the vapor jet. In pancake models, complete evaporation means the disappearance of mass and a complete stop of motion. The theoretical basis of these models needs to be revised.
{"title":"On the Validity of the Pancake Models of the Falls of Cosmic Bodies in the Atmosphere","authors":"V. V. Svettsov","doi":"10.1134/s0038094624700485","DOIUrl":"https://doi.org/10.1134/s0038094624700485","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">\u0000<b>Abstract</b>—</h3><p>Semianalytical pancake models published in the literature are considered, in which it is assumed that a low-strength, fragmented body, like a liquid, expands during flight in the atmosphere and, while maintaining a certain simple shape and increasing the cross-sectional area, decelerates at much higher altitudes than a strong body. Individual models differ in the rate of increase in the transverse size of the body. For comparison with the models, hydrodynamic simulations of falls of liquid bodies with a diameter of 40 m in the Earth’s atmosphere were carried out without taking into account ablation. Such bodies, before they begin to slow down significantly, break up into fragments. Unlike simple models, while the body remains coherent, it can take on very distorted shapes. Comparison of pancake models with the results of hydrodynamic modeling allows us to determine the most suitable models for assessing the behavior of asteroids in the atmosphere and evaluate the assumptions embedded in them. In hydrodynamic modeling taking into account ablation, as shown by the results published in other works, complete evaporation of the body can first occur and, only then, the braking of the vapor jet. In pancake models, complete evaporation means the disappearance of mass and a complete stop of motion. The theoretical basis of these models needs to be revised.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":null,"pages":null},"PeriodicalIF":0.9,"publicationDate":"2024-08-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141881281","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-08-01DOI: 10.1134/s0038094624700461
D. O. Amorim, T. V. Gudkova
Abstract—
Based on the PREM Earth model, more than a thousand models of the internal structure of Venus have been built, differing in the radius and density of the core, the density of the mantle, the viscosity distribution and rheology. The core radius varies from 2800 to 3600 km, and the density in the mantle and core varies within a few percent of the PREM model values. When calculating tidal Love numbers, Andrade rheology is used to take into account the inelasticity of the mantle. Specifically the values of the Andrade rheological model parameters that best describe the tidal deformation of the Earth are used. This significantly reduces the error when calculating Love numbers. It has been shown that Venus can have an internal solid core only if the composition of the planet is very different from that of Earth. Comparison of the observed values of the moment of inertia and tidal Love number k2 with model values allowed us to conclude that the radius of the core of Venus is with a high probability in the range of 3288 ± 167 km.
{"title":"Earth-Like Models of the Internal Structure of Venus","authors":"D. O. Amorim, T. V. Gudkova","doi":"10.1134/s0038094624700461","DOIUrl":"https://doi.org/10.1134/s0038094624700461","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">\u0000<b>Abstract</b>—</h3><p>Based on the PREM Earth model, more than a thousand models of the internal structure of Venus have been built, differing in the radius and density of the core, the density of the mantle, the viscosity distribution and rheology. The core radius varies from 2800 to 3600 km, and the density in the mantle and core varies within a few percent of the PREM model values. When calculating tidal Love numbers, Andrade rheology is used to take into account the inelasticity of the mantle. Specifically the values of the Andrade rheological model parameters that best describe the tidal deformation of the Earth are used. This significantly reduces the error when calculating Love numbers. It has been shown that Venus can have an internal solid core only if the composition of the planet is very different from that of Earth. Comparison of the observed values of the moment of inertia and tidal Love number <i>k</i><sub>2</sub> with model values allowed us to conclude that the radius of the core of Venus is with a high probability in the range of 3288 ± 167 km.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":null,"pages":null},"PeriodicalIF":0.9,"publicationDate":"2024-08-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141881278","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-08-01DOI: 10.1134/s0038094624700497
E. A. Kulik, T. V. Gudkova
Abstract—
The results of numerical modeling of the values of the Chandler wobble period of Mars have been presented for a set of internal structure models that satisfy all currently available observable data: geodetic (average radius, mass, moment of inertia, tidal Love number k2) and crustal thickness and core radius values obtained from seismic data processing. Andrade rheology was used to take into account inelasticity when calculating model values of the tidal Love number k2 and the Chandler wobble period. It has been shown how the model values of the Love number k2 and the Chandler period depend on the Andrade rheological parameter and the adopted viscosity distribution.
{"title":"Influence of Mantle Inelasticity on the Model Value of the Chandler Wobble Period of Mars","authors":"E. A. Kulik, T. V. Gudkova","doi":"10.1134/s0038094624700497","DOIUrl":"https://doi.org/10.1134/s0038094624700497","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">\u0000<b>Abstract</b>—</h3><p>The results of numerical modeling of the values of the Chandler wobble period of Mars have been presented for a set of internal structure models that satisfy all currently available observable data: geodetic (average radius, mass, moment of inertia, tidal Love number <i>k</i><sub>2</sub>) and crustal thickness and core radius values obtained from seismic data processing. Andrade rheology was used to take into account inelasticity when calculating model values of the tidal Love number <i>k</i><sub>2</sub> and the Chandler wobble period. It has been shown how the model values of the Love number <i>k</i><sub>2</sub> and the Chandler period depend on the Andrade rheological parameter and the adopted viscosity distribution.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":null,"pages":null},"PeriodicalIF":0.9,"publicationDate":"2024-08-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141881280","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-08-01DOI: 10.1134/s003809462470045x
M. L. Litvak, I. G. Mitrofanov, A. B. Sanin, M. V. Dyachkova
Abstract—
The article presents the results of the analysis of data from the Russian neutron spectrometer LEND (Lunar Exploration Neutron Detector), installed aboard NASA’s lunar orbiter LRO (Lunar Reconnaissance Orbiter). An estimate of the content of subsurface water ice in the permanently shadowed region Cabeus-1, located inside the large Cabeus crater in the vicinity of the lunar south pole, has been obtained. The analysis used observations made with the LEND instrument from 2009 to 2023. It is shown that the surface neutron albedo in the vicinity and inside of Cabeus-1 correlates with the relief height and the distribution of average annual temperatures. The average subsurface water ice content over the entire Cabeus-1 region was estimated to be 0.49 ± 0.05% by mass fraction. The maximum value of about 0.7% is observed at the very bottom of the crater on the surface area where the minimum average annual temperature was recorded. This site coincides with the site of the LCROSS (Lunar Crater Observation and Sensing Satellite) impact experiment, which confirmed a significant amount of water ice in the near-surface material of the Moon.
{"title":"Subsurface Water Ice Content in the Cabeus Crater According to Measurements by the LEND Instrument onboard the NASA LRO Orbital Mission","authors":"M. L. Litvak, I. G. Mitrofanov, A. B. Sanin, M. V. Dyachkova","doi":"10.1134/s003809462470045x","DOIUrl":"https://doi.org/10.1134/s003809462470045x","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">\u0000<b>Abstract</b>—</h3><p>The article presents the results of the analysis of data from the Russian neutron spectrometer LEND (Lunar Exploration Neutron Detector), installed aboard NASA’s lunar orbiter LRO (<i>Lunar Reconnaissance Orbiter</i>). An estimate of the content of subsurface water ice in the permanently shadowed region Cabeus-1, located inside the large Cabeus crater in the vicinity of the lunar south pole, has been obtained. The analysis used observations made with the LEND instrument from 2009 to 2023. It is shown that the surface neutron albedo in the vicinity and inside of Cabeus-1 correlates with the relief height and the distribution of average annual temperatures. The average subsurface water ice content over the entire Cabeus-1 region was estimated to be 0.49 ± 0.05% by mass fraction. The maximum value of about 0.7% is observed at the very bottom of the crater on the surface area where the minimum average annual temperature was recorded. This site coincides with the site of the LCROSS (<i>Lunar Crater Observation and Sensing Satellite</i>) impact experiment, which confirmed a significant amount of water ice in the near-surface material of the Moon.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":null,"pages":null},"PeriodicalIF":0.9,"publicationDate":"2024-08-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141881282","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-07-12DOI: 10.1134/s0038094624700254
O. L. Vaisberg, A. Yu. Shestakov, R. N. Zhuravlev, D. N. Morozova, A. Ramazan
Abstract—
High temporal resolution of measurements of the magnetic field and plasma of Mars is provided by observations on the Mars Atmosphere and Volatile Evolution (MAVEN; Jakosky et al., 2015) satellite, making it possible to analyze thin layers of the plasma envelope of Mars. This paper describes the magnetic structure associated with the daytime Martian magnetopause. It was shown that the solar wind passing through the shock wave on the dayside of Mars does not directly interact with the Martian ionosphere. A layer of plasma and magnetic field 200–300 km thick forms the daytime magnetosphere, which is the region between the magnetosheath and the ionosphere (Vaisberg and Shuvalov, 2020). There are two types of daytime magnetosphere: (1) the more common type of magnetosphere consists of heated and accelerated O+ ions and ({text{O}}_{2}^{ + }), located between the ionosphere and the flowing hot stream of Mars; (2) another type of daytime magnetosphere consists of accelerated O+ ions and ({text{O}}_{2}^{ + }) in the magnetosheath, where they form a continuing accelerated beam, forming a plume. Between the magnetosheath and the magnetosphere there is a magnetic structure that rotates, almost without changing its size. This structure is located in the second part of the np/(np + nh) transition from ~1 to ~10–2. The transition between the magnetosheath and magnetosphere occurs smoothly, both in energy density and in ion composition, with a decrease in the proton flux and an increase in the heavy ion flux.
{"title":"Change in Plasma Composition During the Rotation of the Magnetopause of Mars","authors":"O. L. Vaisberg, A. Yu. Shestakov, R. N. Zhuravlev, D. N. Morozova, A. Ramazan","doi":"10.1134/s0038094624700254","DOIUrl":"https://doi.org/10.1134/s0038094624700254","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">\u0000<b>Abstract</b>—</h3><p>High temporal resolution of measurements of the magnetic field and plasma of Mars is provided by observations on the Mars Atmosphere and Volatile Evolution (<i>MAVEN</i>; Jakosky et al., 2015) satellite, making it possible to analyze thin layers of the plasma envelope of Mars. This paper describes the magnetic structure associated with the daytime Martian magnetopause. It was shown that the solar wind passing through the shock wave on the dayside of Mars does not directly interact with the Martian ionosphere. A layer of plasma and magnetic field 200–300 km thick forms the daytime magnetosphere, which is the region between the magnetosheath and the ionosphere (Vaisberg and Shuvalov, 2020). There are two types of daytime magnetosphere: (1) the more common type of magnetosphere consists of heated and accelerated O<sup>+</sup> ions and <span>({text{O}}_{2}^{ + })</span>, located between the ionosphere and the flowing hot stream of Mars; (2) another type of daytime magnetosphere consists of accelerated O<sup>+</sup> ions and <span>({text{O}}_{2}^{ + })</span> in the magnetosheath, where they form a continuing accelerated beam, forming a plume. Between the magnetosheath and the magnetosphere there is a magnetic structure that rotates, almost without changing its size. This structure is located in the second part of the <i>n</i><sub>p</sub>/(<i>n</i><sub>p</sub> + <i>n</i><sub>h</sub>) transition from ~1 to ~10<sup>–2</sup>. The transition between the magnetosheath and magnetosphere occurs smoothly, both in energy density and in ion composition, with a decrease in the proton flux and an increase in the heavy ion flux.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":null,"pages":null},"PeriodicalIF":0.9,"publicationDate":"2024-07-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141612742","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-07-12DOI: 10.1134/s003809462470031x
M. Yu. Khovrichev, D. A. Bikulova, D. L. Gorshanov
Abstract
The Yarkovsky effect is one of the noticeable factors in the orbital evolution of near-Earth asteroids (NEAs). The A2 non-gravitational parameter describes the corresponding acceleration in the NEA motion model. This parameter can be derived from astrometric observations of the NEA. We present the results of astrometric observations of two NEAs (2010 XC15 and 2014 HK129). The measurements were performed with the MTM-500M telescope (Mountain Astronomical Station of the Pulkovo Observatory). The modified Gaia star apparent approach technique was applied. As a result, the astrometric accuracy of our observations reached the 0.05 arcsec level. It allowed us to estimate the A2 values of the 2010 XC15 asteroid: –139.5 × 10–15 ± 20.2 × 10–15 au/d2. It is in good agreement with the NASA JPL estimate for this asteroid. The 2014 HK129 A2 parameter formal value extracted from our data is 61.3 × 10–15 ± 1583.4 × 10–15 au/d2. Introduction of this A2 value into the asteroid motion model provides a significant decrease (about 0.05–0.1 arcsec) of the (O–C) values for the first epoch of 2014 HK129 observations. It can be considered as faint evidence of the reality of Yarkovsky drift for the 2014 HK129 asteroid.
{"title":"Calculation of the Non-Gravitational A2 Parameter Using Ground-Based Observations of the Apparent Close Approaches between Near-Earth Asteroids and Gaia Stars","authors":"M. Yu. Khovrichev, D. A. Bikulova, D. L. Gorshanov","doi":"10.1134/s003809462470031x","DOIUrl":"https://doi.org/10.1134/s003809462470031x","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">Abstract</h3><p>The Yarkovsky effect is one of the noticeable factors in the orbital evolution of near-Earth asteroids (NEAs). The A<sub>2</sub> non-gravitational parameter describes the corresponding acceleration in the NEA motion model. This parameter can be derived from astrometric observations of the NEA. We present the results of astrometric observations of two NEAs (2010 XC15 and 2014 HK129). The measurements were performed with the MTM-500M telescope (Mountain Astronomical Station of the Pulkovo Observatory). The modified Gaia star apparent approach technique was applied. As a result, the astrometric accuracy of our observations reached the 0.05 arcsec level. It allowed us to estimate the A<sub>2</sub> values of the 2010 XC15 asteroid: –139.5 × 10<sup>–15</sup> ± 20.2 × 10<sup>–15</sup> au/d<sup>2</sup>. It is in good agreement with the NASA JPL estimate for this asteroid. The 2014 HK129 A<sub>2</sub> parameter formal value extracted from our data is 61.3 × 10<sup>–15</sup> ± 1583.4 × 10<sup>–15</sup> au/d<sup>2</sup>. Introduction of this A<sub>2</sub> value into the asteroid motion model provides a significant decrease (about 0.05–0.1 arcsec) of the (O–C) values for the first epoch of 2014 HK129 observations. It can be considered as faint evidence of the reality of Yarkovsky drift for the 2014 HK129 asteroid.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":null,"pages":null},"PeriodicalIF":0.9,"publicationDate":"2024-07-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141612868","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-07-12DOI: 10.1134/s0038094624700266
T. A. Gornostaeva, P. M. Kartashov, A. V. Mokhov, A. P. Rybchuk, A. T. Basilevsky
Abstract—
A comparative study of impact glasses from the Lonar crater, located on the Deccan basalt plateau, India, and impact glasses from lunar regolith delivered by the Soviet automatic stations (AS) Luna-16 and Luna-24 (Sea of Plenty and Sea of Crises) was carried out. Numerous natural alloys (Cu3Ni2, Ni2Cu and Ni3Cu) that were previously unknown in nature were discovered in the impactites of the Lonar crater and the regolith of the Moon. The discovery of such alloys expands the area of isomorphism in the Cu–Ni system. As a result of a comparison of impactites of the Earth and the Moon, similarities were discovered in the composition, size and morphology of particles of copper–nickel alloys, which may be an indicator of impact processes. One of the possible mechanisms for the formation of Ni–Cu particles was condensation from a gas–plasma cloud. A possible source of material for Cu–Ni alloys was both the impactor material and the target material.
{"title":"Natural Alloys of the Cu–Ni System from Impactites of the Lonar Crater (India) and Lunar Regolith","authors":"T. A. Gornostaeva, P. M. Kartashov, A. V. Mokhov, A. P. Rybchuk, A. T. Basilevsky","doi":"10.1134/s0038094624700266","DOIUrl":"https://doi.org/10.1134/s0038094624700266","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">\u0000<b>Abstract</b>—</h3><p>A comparative study of impact glasses from the Lonar crater, located on the Deccan basalt plateau, India, and impact glasses from lunar regolith delivered by the Soviet automatic stations (AS) <i>Luna-16</i> and <i>Luna-24</i> (Sea of Plenty and Sea of Crises) was carried out. Numerous natural alloys (Cu<sub>3</sub>Ni<sub>2</sub>, Ni<sub>2</sub>Cu and Ni<sub>3</sub>Cu) that were previously unknown in nature were discovered in the impactites of the Lonar crater and the regolith of the Moon. The discovery of such alloys expands the area of isomorphism in the Cu–Ni system. As a result of a comparison of impactites of the Earth and the Moon, similarities were discovered in the composition, size and morphology of particles of copper–nickel alloys, which may be an indicator of impact processes. One of the possible mechanisms for the formation of Ni–Cu particles was condensation from a gas–plasma cloud. A possible source of material for Cu–Ni alloys was both the impactor material and the target material.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":null,"pages":null},"PeriodicalIF":0.9,"publicationDate":"2024-07-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141612653","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-07-12DOI: 10.1134/s0038094624700333
Maocheng Qian, Fabao Yan, Pengyan Zhang, Bo Li, Zhongchen Wu
Abstract
Mars has nearly ideal conditions for CO2 dissociation by glow discharge plasmas. The directly generation of O2 and CO on Mars was considered to be feasible and practical for in situ resource utilization of Martian atmosphere to get respirable O2 and fuel. In this paper, we conduct several experiments under simulated Martian conditions to investigate the process and how the key parameters effect the generation of O2 and CO in CO2 glow discharge reactions. The yields of new products (i.e., O2 and CO) under various gas discharge work parameters (i.e., discharge power, frequency, voltage, gap between the discharge plane electrodes and gas pressure) were systematically investigated. The reaction mechanism and reaction path of CO2 glow discharge has been discussed. In our study the max yield of O2 by CO2 discharge dissociation was got about 21.8 g/h at 168 W which is very close to that of NASA MOXIE (Mars Oxygen In-Situ Resource Utilization Experiment) at the same power. Our results showed the great potentiality of glow discharge for the practicable technology of O2 and CO generation for in-situ resource utilization on Mars.
摘要 火星具有近乎理想的辉光放电等离子体解离二氧化碳的条件。在火星上直接生成 O2 和 CO 被认为是对火星大气进行就地资源利用以获得可吸入 O2 和燃料的可行方法。在本文中，我们在模拟火星条件下进行了多项实验，研究二氧化碳辉光放电反应中生成 O2 和 CO 的过程以及关键参数对其的影响。系统研究了不同气体放电工作参数（即放电功率、频率、电压、放电面电极间隙和气体压力）下新产物（即 O2 和 CO）的产量。讨论了 CO2 辉光放电的反应机理和反应路径。在我们的研究中，二氧化碳放电解离产生的 O2 在 168 W 时的最大产量约为 21.8 g/h，与美国宇航局 MOXIE（火星氧原地资源利用实验）在相同功率下的产量非常接近。我们的研究结果表明，辉光放电在火星原地资源利用的氧气和一氧化碳生成实用技术方面具有巨大潜力。
{"title":"The Generation of O2 and CO by CO2 Glow Discharge for In-Situ Martian Atmospheric Utilization","authors":"Maocheng Qian, Fabao Yan, Pengyan Zhang, Bo Li, Zhongchen Wu","doi":"10.1134/s0038094624700333","DOIUrl":"https://doi.org/10.1134/s0038094624700333","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">Abstract</h3><p>Mars has nearly ideal conditions for CO<sub>2</sub> dissociation by glow discharge plasmas. The directly generation of O<sub>2</sub> and CO on Mars was considered to be feasible and practical for in situ resource utilization of Martian atmosphere to get respirable O<sub>2</sub> and fuel. In this paper, we conduct several experiments under simulated Martian conditions to investigate the process and how the key parameters effect the generation of O<sub>2</sub> and CO in CO<sub>2</sub> glow discharge reactions. The yields of new products (i.e., O<sub>2</sub> and CO) under various gas discharge work parameters (i.e., discharge power, frequency, voltage, gap between the discharge plane electrodes and gas pressure) were systematically investigated. The reaction mechanism and reaction path of CO<sub>2</sub> glow discharge has been discussed. In our study the max yield of O<sub>2</sub> by CO<sub>2</sub> discharge dissociation was got about 21.8 g/h at 168 W which is very close to that of NASA MOXIE (Mars Oxygen In-Situ Resource Utilization Experiment) at the same power. Our results showed the great potentiality of glow discharge for the practicable technology of O<sub>2</sub> and CO generation for in-situ resource utilization on Mars.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":null,"pages":null},"PeriodicalIF":0.9,"publicationDate":"2024-07-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141612740","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-07-12DOI: 10.1134/s0038094624700321
Lu Liu, Qiao Chen, Jianguo Yan, Liangliang Yu, Marco Fenucci, Mao Ye, Zhen Zhong, Denggao Qiu, Jean-Pierre Barriot
Abstract
The Chinese small body exploration mission Tianwen-2 is aimed at sampling the near-Earth, fast-rotating asteroid (469219) Kamo`oalewa and returning the samples to Earth. Characterisation of the currently unknown physical properties of Kamo`oalewa in the pre-mission phase would support mission implementation. In this study, we preliminarily estimate the surface thermal inertia of Kamo`oalewa using a statistical method, based on the Yarkovsky-related orbital drift of (–6.155 ± 1.758) × 10-3 au/Myr for Kamo`oalewa obtained in our previous work. A reasonable estimate of the surface thermal inertia obtained is (402.05_{{ - 194.37}}^{{ + 376.29}}) J K–1 m–2 s–1/2. This low value suggests the presence of coarse regolith on the surface of Kamo`oalewa or its nature as a porous rock. The regolith potentially present on the surface of Kamo`oalewa may have millimetre- to decimetre-sized grains with cohesive strengths varying from ~0.76 to ~0.045 Pa. If Kamo`oalewa is a porous rock, its porosity is expected to range from ~20 to 50%, corresponding to tensile strengths of ~1.3 to 11.5 MPa. This study provides preliminary insights into the surface thermal inertia of Kamo`oalewa from a statistical viewpoint, which may facilitate the Tianwen-2 mission.
{"title":"Surface Thermal Inertia of Near-Earth Asteroid (469219) Kamo`oalewa: Statistical Estimation and Implications","authors":"Lu Liu, Qiao Chen, Jianguo Yan, Liangliang Yu, Marco Fenucci, Mao Ye, Zhen Zhong, Denggao Qiu, Jean-Pierre Barriot","doi":"10.1134/s0038094624700321","DOIUrl":"https://doi.org/10.1134/s0038094624700321","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">Abstract</h3><p>The Chinese small body exploration mission Tianwen-2 is aimed at sampling the near-Earth, fast-rotating asteroid (469219) Kamo`oalewa and returning the samples to Earth. Characterisation of the currently unknown physical properties of Kamo`oalewa in the pre-mission phase would support mission implementation. In this study, we preliminarily estimate the surface thermal inertia of Kamo`oalewa using a statistical method, based on the Yarkovsky-related orbital drift of (–6.155 ± 1.758) × 10<sup>-3</sup> au/Myr for Kamo`oalewa obtained in our previous work. A reasonable estimate of the surface thermal inertia obtained is <span>(402.05_{{ - 194.37}}^{{ + 376.29}})</span> J K<sup>–1</sup> m<sup>–2</sup> s<sup>–1/2</sup>. This low value suggests the presence of coarse regolith on the surface of Kamo`oalewa or its nature as a porous rock. The regolith potentially present on the surface of Kamo`oalewa may have millimetre- to decimetre-sized grains with cohesive strengths varying from ~0.76 to ~0.045 Pa. If Kamo`oalewa is a porous rock, its porosity is expected to range from ~20 to 50%, corresponding to tensile strengths of ~1.3 to 11.5 MPa. This study provides preliminary insights into the surface thermal inertia of Kamo`oalewa from a statistical viewpoint, which may facilitate the Tianwen-2 mission.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":null,"pages":null},"PeriodicalIF":0.9,"publicationDate":"2024-07-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141612743","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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