684 research outputs found
Interplanetary Sample Return Missions Using Radioisotope Electric Propulsion
Solar electric propulsion (SEP) is being used for a variety of planetary missions sponsored by ESA, JAXA, and NASA and nuclear electric propulsion (NEP) is being considered for future, flagship-class interplanetary missions. Radioisotope electric propulsion (REP) has recently been shown to effectively complement SEP and NEP for missions to high-AU targets with modest payload requirements. This paper investigates the application of an advanced REP for a sample return from the comet Tempel 1. A set of mission and system parameters are varied with the goal of quantifying their impact on total mission payload. Mission parameters considered include trip-time and Earth return entry interface speed of the sample return system. System parameters considered include launch vehicle, power level of spacecraft at beginning of mission, and thruster specific impulse. For the baseline case of Atlas 401 and REP power level of 750 W, the mission time was 12 years, the payload was 144 kg, and the missions optimized to a single specific impulse generally within Hall ion thruster range. Other cases were investigated in support of graduate studies, and include the larger Atlas 551 launch vehicle and extended power level to 1 kW. The Atlas 551 cases tended to optimize dual specific impulses generally in the Hall ion thruster range for both legs of the mission. A power level of at least 1-kW and trip-time of approximately 11 years was required to obtain a total science payload close to 320 kg for the Atlas 401 launch vehicle. An Atlas 551 launch vehicle yielded a science payload of approximately 540 kg for the case of 1-kW of power and an 11-year trip time, and nearly 250 kg of science payload for the case of 1-kW of power and a 6-year trip time. Results are also reported indicating the performance ramifications of meeting a reduced Earth entry interface velocity constraint
Determining the Magnetic Field Orientation of Coronal Mass Ejections from Faraday Rotation
We describe a method to measure the magnetic field orientation of coronal
mass ejections (CMEs) using Faraday rotation (FR). Two basic FR profiles,
Gaussian-shaped with a single polarity or "N"-like with polarity reversals, are
produced by a radio source occulted by a moving flux rope depending on its
orientation. These curves are consistent with the Helios observations,
providing evidence for the flux-rope geometry of CMEs. Many background radio
sources can map CMEs in FR onto the sky. We demonstrate with a simple flux rope
that the magnetic field orientation and helicity of the flux rope can be
determined 2-3 days before it reaches Earth, which is of crucial importance for
space weather forecasting. An FR calculation based on global
magnetohydrodynamic (MHD) simulations of CMEs in a background heliosphere shows
that FR mapping can also resolve a CME geometry curved back to the Sun. We
discuss implementation of the method using data from the Mileura Widefield
Array (MWA).Comment: 22 pages with 9 figures, accepted for publication in Astrophys.
Flow and Transport in Regions with Aquatic Vegetation
This review describes mean and turbulent flow and mass transport in the presence of aquatic vegetation. Within emergent canopies, the turbulent length scales are set by the stem diameter and spacing, and the mean flow is determined by the distribution of the canopy frontal area. Near sparse submerged canopies, the bed roughness and near-bed turbulence are enhanced, but the velocity profile remains logarithmic. For dense submerged canopies, the drag discontinuity at the top of the canopy generates a shear layer, which contains canopy-scale vortices that control the exchange of mass and momentum between the canopy and the overflow. The canopy-scale vortices penetrate a finite distance into the canopy, δe, set by the canopy drag. This length scale segregates the canopy into two regions: The upper canopy experiences energetic turbulent transport, controlled by canopy-scale vortices, whereas the lower canopy experiences diminished transport, associated with the smaller stem-scale turbulence. The canopy-scale vortices induce a waving motion in flexible blades, called a monami.National Science Foundation (U.S.) (EAR 0309188)National Science Foundation (U.S.) (EAR 0125056)National Science Foundation (U.S.) (EAR0738352)National Science Foundation (U.S.) (OCE0751358
Temperature Anisotropy in a Shocked Plasma: Mirror-Mode Instabilities in the Heliosheath
We show that temperature anisotropies induced at a shock can account for
interplanetary and planetary bow shock observations. Shocked plasma with
enhanced plasma beta is preferentially unstable to the mirror mode instability
downstream of a quasi-perpendicular shock and to the firehose instability
downstream of a quasi-parallel shock, consistent with magnetic fluctuations
observed downstream of a large variety of shocks. Our theoretical analysis of
the solar wind termination shock suggests that the magnetic holes observed by
Voyager 1 in the heliosheath are produced by the mirror mode instability. The
results are also of astrophysical interest, providing an energy source for
plasma heating.Comment: 11 pages, 2 figures, accepted for publication in ApJ Letter
Multispacecraft measurement of anisotropic correlation functions in solar wind turbulence
Published versio
Evolution of Near-Sun Solar Wind Turbulence
This paper presents a preliminary analysis of the turbulence spectrum of the
solar wind in the near-Sun region R < 50 Rs, obtained from interplanetary
scintillation measurements with the Ooty Radio Telescope at 327 MHz. The
results clearly show that the scintillation is dominated by density
irregularities of size about 100 - 500 km. The scintillation at the small-scale
side of the spectrum, although significantly less in magnitude, has a flatter
spectrum than the larger-scale dominant part. Furthermore, the spectral power
contained in the flatter portion rapidly increases closer to the Sun. These
results on the turbulence spectrum for R < 50 Rs quantify the evidence for
radial evolution of the small-scale fluctuations (</= 50 km) generated by
Alfven waves.Comment: 8 pages, 5 figures, To appear in "Magnetic Coupling between the
Interior and the Atmosphere of the Sun", eds. S.S. Hasan and R.J. Rutten,
Astrophysics and Space Science Proceedings, Springer-Verlag, Heidelberg,
Berlin, 200
Plasma Depletion and Mirror Waves Ahead of Interplanetary Coronal Mass Ejections
We find that the sheath regions between fast interplanetary coronal mass
ejections (ICMEs) and their preceding shocks are often characterized by plasma
depletion and mirror wave structures, analogous to planetary magnetosheaths. A
case study of these signatures in the sheath of a magnetic cloud (MC) shows
that a plasma depletion layer (PDL) coincides with magnetic field draping
around the MC. In the same event, we observe an enhanced thermal anisotropy and
plasma beta as well as anti-correlated density and magnetic fluctuations which
are signatures of mirror mode waves. We perform a superposed epoch analysis of
ACE and Wind plasma and magnetic field data from different classes of ICMEs to
illuminate the general properties of these regions. For MCs preceded by shocks,
the sheaths have a PDL with an average duration of 6 hours (corresponding to a
spatial span of about 0.07 AU) and a proton temperature anisotropy -1.3, and are marginally unstable to the
mirror instability. For ICMEs with preceding shocks which are not MCs, plasma
depletion and mirror waves are also present but at a reduced level. ICMEs
without shocks are not associated with these features. The differences between
the three ICME categories imply that these features depend on the ICME geometry
and the extent of upstream solar wind compression by the ICMEs. We discuss the
implications of these features for a variety of crucial physical processes
including magnetic reconnection, formation of magnetic holes and energetic
particle modulation in the solar wind.Comment: fully refereed, accepted for publication in J. Geophys. Re
Cell walls of the dimorphic fungal pathogens Sporothrix schenckii and Sporothrix brasiliensis exhibit bilaminate structures and sloughing of extensive and intact layers
This work was supported by the Fundação Carlos Chagas de Amparo à Pesquisa do Estado do Rio de Janeiro (FAPERJ), grants E-26/202.974/2015 and Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq), grants 229755/2013-5, Brazil. LMLB is a senior research fellow of CNPq and Faperj. NG acknowledged support from the Wellcome Trust (Trust (097377, 101873, 200208) and MRC Centre for Medical Mycology (MR/N006364/1). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript.Peer reviewedPublisher PD
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In-street wind direction variability in the vicinity of a busy intersection in central London
We present results from fast-response wind measurements within and above a busy intersection between two street canyons (Marylebone Road and Gloucester Place) in Westminster, London taken as part of the DAPPLE (Dispersion of Air Pollution and Penetration into the Local Environment; www.dapple.org.uk) 2007 field campaign. The data reported here were collected using ultrasonic anemometers on the roof-top of a building adjacent to the intersection and at two heights on a pair of lamp-posts on opposite sides of the intersection. Site characteristics, data analysis and the variation of intersection flow with the above-roof wind direction (θref) are discussed. Evidence of both flow channelling and recirculation was identified within the canyon, only a few metres from the intersection for along-street and across-street roof-top winds respectively. Results also indicate that for oblique rooftop flows, the intersection flow is a complex combination of bifurcated channelled flows, recirculation and corner vortices. Asymmetries in local building geometry around the intersection and small changes in the background wind direction (changes in 15-min mean θref of 5–10 degrees) were also observed to have profound influences on the behaviour of intersection flow patterns. Consequently, short time-scale variability in the background flow direction can lead to highly scattered in-street mean flow angles masking the true multi-modal features of the flow and thus further complicating modelling challenges
Kinetic Turbulence
The weak collisionality typical of turbulence in many diffuse astrophysical
plasmas invalidates an MHD description of the turbulent dynamics, motivating
the development of a more comprehensive theory of kinetic turbulence. In
particular, a kinetic approach is essential for the investigation of the
physical mechanisms responsible for the dissipation of astrophysical turbulence
and the resulting heating of the plasma. This chapter reviews the limitations
of MHD turbulence theory and explains how kinetic considerations may be
incorporated to obtain a kinetic theory for astrophysical plasma turbulence.
Key questions about the nature of kinetic turbulence that drive current
research efforts are identified. A comprehensive model of the kinetic turbulent
cascade is presented, with a detailed discussion of each component of the model
and a review of supporting and conflicting theoretical, numerical, and
observational evidence.Comment: 31 pages, 3 figures, 99 references, Chapter 6 in A. Lazarian et al.
(eds.), Magnetic Fields in Diffuse Media, Astrophysics and Space Science
Library 407, Springer-Verlag Berlin Heidelberg (2015
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