Carol S. Paty

Cassini detection of Enceladus' cold water‐group plume ionosphere

This study reports direct detection by the Cassini plasma spectrometer of freshly-produced water-group ions (O{sup +}, OH{sup +}, H{sub 2}O{sup +}, H{sub 3}O{sup +}) and heavier water dimer ions (H{sub x}O{sub 2}{sup +}) very close to Enceladus and where the plasma begins to emerge from the Enceladus plume The data wcre obtained during two close (52 and 25 km) flybys of Enceladus in 2008, and are similar to ion data in cometary comas. The ions are observed in detectors looking in the Cassini ram direction at energies consistent with the Cassini speed, indicating a nearly stagnant plasma flow in the plume. North of Enceladus the plasma slowing commences about 4 to 6 Enceladus radii away, while south of Enccladus signatures ofthe interaction are detected as far as 22 Enceladus radii away.

Electrodynamics of the Martian dynamo region near magnetic cusps and loops

Strong and inhomogeneous remanent magnetization on Mars results in a complex pattern of crustal magnetic fields. The geometry and topology of these fields lead to atmospheric electrodynamic structures that are unique among the bodies of the solar system. In the atmospheric dynamo region (∼100−250 km altitude), ions depart from the gyropath due to collisions with neutral particles, while electron motion remains governed by electromagnetic drift. This differential motion of the charge carriers generates electric currents, which induce a perturbation field. The electromagnetic changes ultimately alter the behavior of the local ionosphere beyond the dynamo region. Here we use multifluid modeling to investigate the dynamics around an isolated magnetic cusp and around magnetic loops or arcades representative of the magnetic topology near, for example, Terra Sirenum. Our results show consistent, circular patterns in the electric current around regions with high local field strength, with possible consequences on atmospheric escape of charged particles.

On wind-driven electrojets at magnetic cusps in the nightside ionosphere of Mars

Mars has a complex magnetic topology where crustal magnetic fields can interact with the solar wind magnetic field to form magnetic cusps. On the nightside, solar wind electron precipitation can produce enhanced ionization at cusps while closed field regions adjacent to cusps can be devoid of significant ionization. Using an electron transport model, we calculate the spatial structure of the nightside ionosphere of Mars using Mars Global Surveyor electron measurements as input. We find that localized regions of enhanced ionospheric density can occur at magnetic cusps adjacent to low density regions. Under this configuration, thermospheric winds can drive ionospheric electrojets. Collisional ions move in the direction of the neutral winds while magnetized electrons move perpendicular to the wind direction. This difference in motion drives currents and can lead to charge accumulation at the edges of regions of enhanced ionization. Polarization fields drive secondary currents which can reinforce the primary currents leading to electrojet formation. We estimate the magnitude of these electrojets and show that their magnetic perturbations can be detectable from both orbiting spacecraft and the surface. The magnitude of the electrojets can vary on diurnal and annual time scales as the strength and direction of the winds vary. These electrojets may lead to localized Joule heating, and closure of these currents may require field-aligned currents which may play a role in high altitude acceleration processes.

Application of adaptive weights to intelligent information systems: An intelligent transportation system as a case study

Optimization of information feedback technologies is very important for many socioeconomic systems such as stock markets and traffic systems aiming to make full use of resources. In this paper, we propose an adaptive weight method, which has potential value for a variety of information processing contexts. We apply this adaptive weight method to an intelligent transportation system (ITS) as a case study. A feedback strategy named Improved Congestion Coefficient Feedback Strategy (ICCFS) is introduced based on a two-route scenario in which dynamic information can be generated and displayed on the roadside in order to enable drivers to make an informed route decision. Our model incorporates the effects of adaptability into the cellular automaton models of traffic flow. Simulations demonstrate that adopting this optimal information feedback strategy provides a high efficiency in controlling spatial distribution of traffic patterns when compared with the three other information feedback strategies, i.e., Travel Time Feedback Strategy (TTFS), Mean Velocity Feedback Strategy (MVFS) and Congestion Coefficient Feedback Strategy (CCFS).

Heating of ions by low-frequency Alfvén waves in partially ionized plasmas

In the solar atmosphere, the chromospheric and coronal plasmas are much hotter than the visible photosphere. The heating of the solar atmosphere, including the partially ionized chromosphere and corona, remains largely unknown. In this letter, we demonstrate that the ions can be substantially heated by Alfven waves with very low frequencies in partially ionized low-beta plasmas. This differs from other Alfven wave related heating mechanisms such as ion-neutral collisional damping of Alfven waves and heating described by previous work on resonant Alfven wave heating. We find that the nonresonant Alfven wave heating is less efficient in partially ionized plasmas than when there are no ion-neutral collisions, and the heating efficiency depends on the ratio of the ion-neutral collision frequency to the ion gyrofrequency.

Uncovering local magnetospheric processes governing the morphology and variability of Ganymede's aurora using three-dimensional multifluid simulations of Ganymede's magnetosphere

We investigate local magnetospheric processes governing the morphology and variability of Ganymedes aurora depending on its position with respect to the center of the Jovian plasma sheet. We couple an existing three-dimensional multifluid simulation to a new aurora brightness model developed for this study. With this, we are able to qualitatively and quantitatively show that the short- and long-period variabilities observed in Ganymedes auroral footprint at Jupiter are also predicted to be present in the brightness and morphology of the aurora at Ganymede. We also examine the relationship between acceleration structures and precipitation of electrons in Ganymedes neutral atmosphere by looking at the component of the electric field parallel to Ganymedes magnetic field. Our results confirm that regions of electron accelerations coincide with regions of brightest auroral emissions, as expected. Finally, we identify the likely source regions of electrons generating the aurora at Ganymede and discuss the plasma dynamic mechanisms likely responsible for these accelerations.

Effect of plasma torus density variations on the morphology and brightness of the Io footprint

We develop a 2-D-layered model of the Io plasma torus to study the apparent “shutoff” of the Io footprint in 2007, when it disappeared beneath a region of diffuse emissions, roughly coincident with a massive eruption of Tvashtar Paterae. First, we investigate the effects of Ios location in the plasma torus and validate our model results against Hubble UV observations of the Io footprint. We are able to qualitatively reproduce variations in the morphology of the footprint due to Ios changing latitudinal location with respect to the center of the plasma torus, capturing the bright leading spot and the dimmer tail. Then, we consider the effects of an increase in the local plasma density on the brightness and morphology of the Io footprint. Our results show a correlation between a local density increase in the plasma torus and the dimming of the Io footprint as observed in 2007. In particular, we find that a local density enhancement at Io of fivefold compared to the nominal value is sufficient to produce the observed shutoff of the footprint.

Response to "Comment on 'Heating of ions by low-frequency Alfven waves in partially ionized plasmas'" (Phys. Plasmas 18, 084703 (2011))

The calculation of temperature in a plasma system that is not in thermal equilibrium remains a topic of debate. In our article [Dong and Paty, Phys. Plasmas 18, 030702 (2011)] we use the average kinetic energy to calculate the “kinetic temperature” in a non-equilibrium system to quantify the heating of ions by low-frequency Alfven waves in a partially ionized plasma (i.e., where collisions with neutrals can not be ignored). We implement a method previously used by Wang, Wu and Yoon [Wang, Wu and Yoon, Phys. Rev. Lett. 96, 125001 (2006)] and several others studying the effects of low frequency Alfven waves in collisionless plasmas. This method is appropriate for several reasons discussed in this response. Most notably, we implement it to investigate heating of the plasma population since the bulk velocity of the particle ensemble perpendicular to the ambient magnetic field remains zero during the numerical experiment.

Statistical study of ICME effects on Mercury's magnetospheric boundaries and northern cusp region from MESSENGER†

This paper presents a systematic investigation of the large-scale processes in Mercurys magnetosphere during interplanetary coronal mass ejections (ICMEs) using observations from the MESSENGER mission. We study the motion of the bow shock and magnetopause boundaries, quantify the magnetospheric compression, and characterize the size, extent, and plasma pressure of the northern cusp region, and the plasma precipitation to the surface. During ICMEs, the magnetopause was substantially compressed, as the subsolar stand-off distance from the center of the planet was reduced by ∼15% compared with the value during nominal solar wind conditions, and the magnetopause reached the surface of the planet ∼30% of the time. On the other hand, the bow shock under ICME conditions was located farther from the planet than for nominal solar wind conditions. The cusp was observed to extend ∼10∘ further equatorward and 2 h wider in local time. In addition, the average plasma pressure in the cusp was more than double that determined under nominal conditions. For the most extreme cases, the particle precipitation to the surface was an order of magnitude higher than on average. The solar wind ram pressure and the Alfven Mach number are found to be the dominant factors affecting these changes in the magnetosphere, with the IMF direction and the IMF magnetic pressure playing a small, but likely non-negligible role.

Hubble Space Telescope Observations of Variations in Ganymede's Oxygen Atmosphere and Aurora

We present high-sensitivity Hubble Space Telescope (HST) Cosmic Origins Spectrograph and HST Space Telescope Imaging Spectrograph measurements of atmospheric OI 130.4-nm and OI] 135.6-nm emissions at Ganymede, which exhibit significant spatial and temporal variability. These observations represent the first observations of Ganymede using HST Cosmic Origins Spectrograph and of both the leading and trailing hemispheres within a single HST campaign, minimizing the potential influence of long-term changes in the Jovian plasma sheet or in Ganymede’s atmosphere on the comparison of the two hemispheres. The mean disk-averaged OI] 135.6-nm/OI 130.4-nm observed intensity ratio was 2.72 ± 0.57 on the leading hemisphere and 1.42 ± 0.16 on the trailing hemisphere. The observed leading hemisphere ratios are consistent with an O2 atmosphere, but we show that an atomic oxygen component of ~10% is required to produce the observed trailing hemisphere ratios. The excess 130.4-nm emission on the trailing hemisphere relative to that expected for an O2 atmosphere was ~11 R. The O column density required to produce this excess is determined based on previous estimates of the electron density and temperature at Ganymede and exceeds the limit for an optically thin atmosphere. The implication that the O atmosphere is optically thick may be investigated in future by observing Ganymede as it moves into eclipse or by determining the ratio of the individual components within the 130.4-nm triplet.