Cassini CAPS-ELS observations of negative ions in Titan's ionosphere: trends of density with altitude

Observations with the Electron Spectrometer sensor of the Cassini Plasma Spectrometer (CAPS-ELS) have revealed the existence of negative ions in Titan's ionosphere. Negative ions are observed during encounters whenever the instrument points in the ram direction at altitudes 950–1400 km. Complex hydrocarbon and nitrile chemical processes are believed to take place which play a role in haze formation. The heaviest ions observed so far have masses up to 13,800 amu/q. Using data from 34 Titan encounters, we show for the first time negative ion density trends of different mass groups, including total densities, with altitude. We determine peak densities and the associated altitudes at which they are observed and the highest altitudes at which individual mass groups are found

Cassini's floating potential in Titan's ionosphere: 3-D Particle-In-Cell Simulations

Accurate determination of Cassini's spacecraft potential in Titan's ionosphere is important for interpreting measurements by its low energy plasma instruments. Estimates of the floating potential varied significantly, however, between the various different plasma instruments. In this study we utilize 3-D particle-in-cell simulations to understand the key features of Cassini's plasma interaction in Titan's ionosphere. The spacecraft is observed to charge to negative potentials for all scenarios considered, and close agreement is found between the current onto the simulated Langmuir Probe and that observed in Titan's ionosphere. These simulations are therefore shown to provide a viable technique for modeling spacecraft interacting with Titan's dusty ionosphere.Comment: 4 pages, 4 figures, 1 table, accepted for publication at URSI General Assembly and Scientific Symposium 2023, Sapporo, Japa

PENGARUH KUANTITAS LAYANAN DAN KEPERCAYAAN TERHADAP KEPUASAN NASABAH KREDIT MIKRO PADA BANK PT. BTPN ARGAMAKMUR

The purpose of this research were the impact of service quality toward :ustomer satisfaction at BTPN Bank of Argamalcnur Branch, 2J Analyze the impact of irust toward customer satisfaction at BTPN Bank of Argamakmur Branch, 3) Analyze rhe impact of service quality and trust toward customer satisfaction at BTPN Bank of Argamakmur Branch, 4) Identified the variable that had dominance impact toward customer satisfaction at BTPN Bank of Argamakmur Branch. Purpose sampling method ',vas used on this research. The numbers of sampling were 155 respondents. Multiple regression analysis was used as research method on this study. The result of study can be summaries: 1) There was significant impact of service quality toward customer satisfaction at BTPN Bank of Argamakmur Branch with the value of coefficient was 0,467; 2J There was significant impact of tn-rst toward customer satisfaction at BTPN Bank of Argamakmur Branch with the value of coefficient was 0,382,3) There was significant impact of service quality and trust toward customer satisfaction at BTPN Bank of Argamalnnur Branch with the value of inpact was 67 ,2o/o and 32,8o/a of the rest was influence by other factors, 4) Based on the study found that the service quality had more strong impact to customer satisfaction rather than of trust at BTPN Bank of Argamakmur Branch

Discrimination in sports as a gross violation of human rights in Ukraine

The urgency of the problem described in the article is the existence of an ineffective observance mechanism of athletes' and fans' rights in connection with the manifestations of discrimination in sports. Therefore, the purpose of the article is to find ways to improve Ukrainian legislation in terms of protection of human rights from any manifestations of discrimination. To achieve this goal, the system-structural method and the formal-legal method, the method of analysis, the formal-logical method were used. The Ukrainian legislation in the researched field is analyzed. The experience of other countries in combating discrimination in sports has been studied. It is proposed to create an institute of sports ombudsman in Ukraine and stressed the need not to improve the criminal legislation in terms of clarifying the provisions of Article 161 of the Criminal Code of Ukraine. The expediency of establishing administrative liability for non-compliance with anti-discrimination legislation, amending the Code of Ukraine on Administrative Offenses, which, in turn, will facilitate more prompt prosecution for human rights violations in sports. The practical value of the obtained results is that it can be taken as a basis for finding a mechanism to improve the fight against discrimination in sports

Ion and aerosol precursor densities in Titan's ionosphere: A multi-instrument case study

The importance of the heavy ions and dust grains for the chemistry and aerosol formation in Titan's ionosphere has been well established in the recent years of the Cassini mission. In this study we combine independent in situ plasma (Radio Plasma and Wave Science Langmuir Probe (RPWS/LP)) and particle (Cassini Plasma Science Electron Spectrometer, Cassini Plasma Science Ion Beam Spectrometer, and Ion and Neutral Mass Spectrometer) measurements of Titan's ionosphere for selected flybys (T16, T29, T40, and T56) to produce altitude profiles of mean ion masses including heavy ions and develop a Titan-specific method for detailed analysis of the RPWS/LP measurements (applicable to all flybys) to further constrain ion charge densities and produce the first empirical estimate of the average charge of negative ions and/or dust grains. Our results reveal the presence of an ion-ion (dusty) plasma below ~1100 km altitude, with charge densities exceeding the primary ionization peak densities by a factor ≥2 in the terminator and nightside ionosphere (ne/ni ≤ 0.1). We suggest that ion-ion (dusty) plasma may also be present in the dayside ionosphere below 900 km (ne/ni < 0.5 at 1000 km altitude). The average charge of the dust grains (≥1000 amu) is estimated to be between −2.5 and −1.5 elementary charges, increasing toward lower altitudes

Cassini's floating potential in Titan's ionosphere: 3-D particle-in-cell simulations

Accurate determination of Cassini’s spacecraft potential in Titan’s ionosphere is important for interpreting measurements by its low energy plasma instruments. Estimates of the floating potential varied significantly, however, between the various different plasma instruments. In this study we utilize 3-D particle-in-cell simulations to understand the key features of Cassini’s plasma interaction in Titan’s ionosphere. The spacecraft is observed to charge to negative potentials for all scenarios considered, and close agreement is found between the current onto the simulated Langmuir Probe and that observed in Titan’s ionosphere. These simulations are therefore shown to provide a viable technique for modeling spacecraft interacting with Titan’s dusty ionosphere

Cassini's floating potential in Titan's ionosphere: 3-D Particle-In-Cell Simulations

Accurate determination of Cassini's spacecraft potential in Titan's ionosphere is important for interpreting measurements by its low energy plasma instruments. Estimates of the floating potential varied significantly, however, between the various different plasma instruments. In this study we utilize 3-D particle-in-cell simulations to understand the key features of Cassini's plasma interaction in Titan's ionosphere. The spacecraft is observed to charge to negative potentials for all scenarios considered, and close agreement is found between the current onto the simulated Langmuir Probe and that observed in Titan's ionosphere. These simulations are therefore shown to provide a viable technique for modeling spacecraft interacting with Titan's dusty ionosphere.Comment: 4 pages, 4 figures, 1 table, accepted for publication at URSI General Assembly and Scientific Symposium 2023, Sapporo, Japa

Effects of Saturn's magnetospheric dynamics on Titan's ionosphere

We use the Cassini Radio and Plasma Wave Science/Langmuir probe measurements of the electron density from the first 110 flybys of Titan to study how Saturn´s magnetosphere influences Titan´s ionosphere. The data is first corrected for biased sampling due to varying solar zenith angle and solar energy flux (solar cycle effects). We then present results showing that the electron density in Titan´s ionosphere, in the altitude range 1600-2400 km, is increased by about a factor of 2.5 when Titan is located on the nightside of Saturn (Saturn local time (SLT) 21-03 h) compared to when on the dayside (SLT 09-15 h). For lower altitudes (1100-1600 km) the main dividing factor for the ionospheric density is the ambient magnetospheric conditions. When Titan is located in the magnetospheric current sheet, the electron density in Titan´s ionosphere is about a factor of 1.4 higher compared to when Titan is located in the magnetospheric lobes. The factor of 1.4 increase in between sheet and lobe flybys is interpreted as an effect of increased particle impact ionization from 200 eV sheet electrons. The factor of 2.5 increase in electron density between flybys on Saturn´s nightside and dayside is suggested to be an effect of the pressure balance between thermal plus magnetic pressure in Titan´s ionosphere against the dynamic pressure and energetic particle pressure in Saturn´s magnetosphere.Fil: Edberg, N. J. T.. University of Iowa; Estados Unidos. Swedish Institute of Space Physics; SueciaFil: Andrews, D. J.. Swedish Institute of Space Physics; SueciaFil: Bertucci, Cesar. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Gurnett, D. A.. University of Iowa; Estados UnidosFil: Holmberg, M. K. G.. Swedish Institute of Space Physics; SueciaFil: Jackman, C. M.. University Of Southampton; Reino UnidoFil: Kurth, W. S.. University of Iowa; Estados UnidosFil: Menietti, J. D.. University Of Iowa; Estados UnidosFil: Opgenoorth, H. J.. Swedish Institute of Space Physics; SueciaFil: Shebanits, O.. Swedish Institute of Space Physics; SueciaFil: Vigren, E.. Swedish Institute of Space Physics; SueciaFil: Wahlund, J. E.. Swedish Institute of Space Physics; Sueci