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Search indexed NASA NTRS and DOE OSTI research on propulsion, heat transfer, battery materials and energy systems. Follow report and document links to the original sources.

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At least 505 records · Page 28
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DOE OSTI2010

EVIDENCE FOR GENTLY SLOPING PLASMA DENSITY PROFILES IN THE DEEP CORONA: TYPE III OBSERVATIONS

Type III radio bursts are produced near the local electron plasma frequency f{sub p} and near its harmonic 2f{sub p} by fast electrons ejected from the solar active regions and moving through the corona and solar wind. The coronal bursts have dynamic spectra with frequency rapidly falling with time, the typical duration being about 1-3 s. In the present paper, 37 well-defined coronal type III radio bursts (25-450 MHz) are analyzed. The results obtained substantiate an earlier statement that the dependence of the central frequency of the emission on time can be fitted to a power-law model, f(t) {proportional_to} (t - t{sub 0}){sup -{alpha}}, where {alpha} can be as low as 1. In the case of negligible plasma acceleration and conical flow, it means that the electron number density within about 1 solar radius above the photosphere will decrease as r {sup -2}, like in the solar wind. For the data set chosen, the index {alpha} varies in the range from 0.2 to 7 or bigger, with mean and median values of 1.2 and 0.5, respectively. A surprisingly large fraction of events, 84%, have {alpha} {<=} 1.2. These results provide strong evidence that in the type III source regions the electron number density scales as n(r) {proportional_to} (r - r{sub 0}){sup -{beta}}, with minimum, mean, and median {beta} = 2{alpha} of 0.4, 2.4, and 1.0, respectively. Hence, the typical density profiles are more gently sloping than those given by existing empirical coronal models. Several events are found with a wind-like dependence of burst frequency on time. Smaller power-law indices could result from the effects of non-conical geometry of the plasma flow tubes, deceleration of coronal plasma, and/or the curvature of the magnetic field lines. The last effect is shown to be too weak to explain such low power-law indices. A strong tendency is found for bursts from the same group to have similar power-law indices, thereby favoring the hypothesis that they are usually produced by the same source region.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2010

SMEI 3D RECONSTRUCTION OF A CORONAL MASS EJECTION INTERACTING WITH A COROTATING SOLAR WIND DENSITY ENHANCEMENT: THE 2008 APRIL 26 CME

The Solar Mass Ejection Imager (SMEI) has recorded the brightness responses of hundreds of interplanetary coronal mass ejections (CMEs) in the interplanetary medium. Using a three-dimensional (3D) reconstruction technique that derives its perspective views from outward-flowing solar wind, analysis of SMEI data has revealed the shapes, extents, and masses of CMEs. Here, for the first time, and using SMEI data, we report on the 3D reconstruction of a CME that intersects a corotating region marked by a curved density enhancement in the ecliptic. Both the CME and the corotating region are reconstructed and demonstrate that the CME disrupts the otherwise regular density pattern of the corotating material. Most of the dense CME material passes north of the ecliptic and east of the Sun-Earth line: thus, in situ measurements in the ecliptic near Earth and at the Solar-TErrestrial RElations Observatory Behind spacecraft show the CME as a minor density increase in the solar wind. The mass of the dense portion of the CME is consistent with that measured by the Large Angle Spectrometric Coronagraph on board the Solar and Heliospheric Observatory spacecraft, and is comparable to the masses of many other three-dimensionally reconstructed solar wind features at 1 AU observed in SMEI 3D reconstructions.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2010

SEARCHING FOR OVERTURNING CONVECTION IN PENUMBRAL FILAMENTS: SLIT SPECTROSCOPY AT 0.''2 RESOLUTION

Recent numerical simulations of sunspots suggest that overturning convection is responsible for the existence of penumbral filaments and the Evershed flow, but there is little observational evidence of this process. Here, we carry out a spectroscopic search for small-scale convective motions in the penumbra of a sunspot located 5{sup 0} away from the disk center. The position of the spot is very favorable for the detection of overturning downflows at the edges of penumbral filaments. Our analysis is based on measurements of the Fe I 709.0 nm line taken with the Littrow spectrograph of the Swedish 1 m Solar Telescope under excellent seeing conditions. We compute line bisectors at different intensity levels and derive Doppler velocities from them. The velocities are calibrated using a nearby telluric line, with systematic errors smaller than 150 m s{sup -1}. Deep in the photosphere, as sampled by the bisectors at the 80%-88% intensity levels, we always observe blueshifts or zero velocities. The maximum blueshifts reach 1.2 km s{sup -1} and tend to be cospatial with bright penumbral filaments. In the line core, we detect blueshifts for the most part, with small velocities not exceeding 300 m s{sup -1}. Redshifts also occur, but at the level of 100-150 m s{sup -1}, and only occasionally. The fact that they are visible in high layers casts doubts on their convective origin. Overall, we do not find indications of downflows that could be associated with overturning convection at our detection limit of 150 m s{sup -1}. Either no downflows exist, or we have been unable to observe them because they occur beneath {tau} = 1 or the spatial resolution/height resolution of the measurements is still insufficient.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2010

PITCH ANGLE SCATTERING IN THE OUTER HELIOSHEATH AND FORMATION OF THE INTERSTELLAR BOUNDARY EXPLORER RIBBON

The dominant and unexpected feature in the first Interstellar Boundary EXplorer (IBEX) maps is a ribbon of the enhanced energetic neutral atom (ENA) emissions. Presenting the first results from IBEX, McComas et al. identified six possible mechanisms of ribbon formation. One of the mechanisms, the so-called secondary ENA mechanism, was already quantitatively elaborated by Heerikhuisen et al., and they successfully reproduced the main features of the ribbon. We further study the 'secondary ENA' mechanism by quantifying a previously omitted stage of the proton evolution between two consecutive acts of the charge-exchange in the outer heliosheath (OHS). The main findings can be summarized as follows. (1) The neutrals supplied by the supersonic near-equatorial solar wind dominate the near-equatorial source of the keV ENAs in the OHS compared to the inner heliosheath contribution. (2) The ribbon of the observed width can be produced even if only the large-scale ({approx}10{sup 2}-10{sup 4} AU) interstellar turbulence operates but the resulting pitch angle distribution functions (PADFs) are unstable with respect to the ion cyclotron wave generation around the locus where the line of sight from IBEX to the ribbon is perpendicular to the interstellar magnetic field beyond the heliopause. (3) A combination of the large-scale interstellar turbulence and a small-scale ({approx}10{sup -5}to10{sup -4} AU) turbulence generated by an unstable PADF of the energetic protons is able to make PADF marginally stable. In this case, the ribbon is still narrow because only a small part of the proton phase space distribution function can resonate with a locally generated ion cyclotron turbulence. (4) A concurrent operation of the large-scale interstellar turbulence and the locally generated small-scale turbulence might be responsible for the localized emission structures observed in the IBEX ribbon.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2010

OBSERVED CORE OF A GRADUAL SOLAR ENERGETIC PARTICLE EVENT

Using space-borne particle and EUV detection and radio spectrograms from both ground-based and space-borne instruments, we study the first phase of the major solar energetic particle (SEP) event associated with the western solar flare and fast and wide coronal mass ejection (CME) on 2000 April 4. The SEP event being observed at the magnetic connection to the eruption's center starts with deka-MeV nucl{sup -1} helium- and relativistic electron-rich production from coronal sources identified with the electromagnetic diagnostics and the SEP event modeling. The broadband observations and modeling of the initial phase of the 'well-connected' major SEP event support the idea that acceleration of SEPs starts in the helium-rich plasma of the eruption's core in association with coronal shocks and magnetic reconnections caused by the CME liftoff, and that the coronal component dominates during the first hour of the SEP event considered, not yet being shielded by the CME bow shock in the solar wind. The first phase of the SEP event is followed by a second phase of SEP production associated with a decelerating CME-driven shock wave in the solar wind, which accelerates ions from a distinct, helium-poor seed particle population that may originate from the CME interaction with a coronal streamer.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2011

EVIDENCE FOR THE FULL HARD X-RAY SPECTRAL SIGNATURE OF NONUNIFORM IONIZATION IN A SOLAR FLARE

The hard X-ray (HXR) emission from solar flares is observed primarily from the footpoints of flare magnetic loops, where nonthermal electrons are understood to emit thick-target bremsstrahlung as they stream from the fully ionized hot corona to the denser, cooler, and partially ionized chromosphere. The change in the plasma ionization along the path of the electrons should result in a characteristic upward break and corresponding flattening of the X-ray spectrum with increasing energy at lower energies, and a downward break at higher energies. Due to the presence of thermal emission, the upward break usually cannot be observed. We report the first evidence for both breaks in spectra measured with the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) during the GOES X1.2 class flare that happened on 2002 October 31. The RHESSI X-ray spectral analysis shows both the breakup at {approx}49 keV and the breakdown at {approx}134 keV at the HXR peak time. The time evolution of both breaks also agrees with the nonuniform ionization (NUI) model. Other possible explanations for the breaks are considered, but the NUI model provides the simplest explanation for the spectral shape and its time evolution. We find that the average column density of the fully ionized plasma changed from 2 x10{sup 19} cm{sup -2} in the rise phase to 7 x10{sup 21} cm{sup -2} after the peak. This indicates that plasma in the target was heated and became ionized during the flare, in agreement with heating by the nonthermal electrons and chromospheric evaporation expected in the collisional thick-target model.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2011

TEMPORAL RELATION BETWEEN THE DISAPPEARANCE OF PENUMBRAL FINE-SCALE STRUCTURE AND EVERSHED FLOW

We investigate the temporal relation between the Evershed flow, dot-like bright features (penumbral grain), the complex magnetic field structure, and dark lanes (dark core) along bright filaments in a sunspot penumbra. We use a time series of high spatial resolution photospheric intensity, vector magnetic field maps, and Doppler velocity maps obtained with the Solar Optical Telescope aboard the Hinode spacecraft. We conclude that the appearance and disappearance of the Evershed flow and penumbra grains occur at nearly the same time and are associated with changes of the inclination angle of the magnetic field from vertical to more horizontal. This supports the idea that Evershed flow is a result of thermal convection in the inclined field lines. The dark core of the bright penumbral filament also appears coincidental with the Evershed flow. However, the dark-cored bright filament survives at least for 10-20 minutes after the disappearance of the Evershed flow. The heat input into the bright filament continues even after the end of heat transfer by the Evershed flow. This suggests that local heating along the bright filament is important for maintaining its brightness, in addition to heat transfer by the Evershed flow.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2011

FIRST SKY MAP OF THE INNER HELIOSHEATH TEMPERATURE USING IBEX SPECTRA

Analysis of the IBEX-Hi Energetic Neutral Atom spectra reveals, for the first time, the sky map of the source ion temperatures. The solar wind exists in non-equilibrium stationary states and can be described by kappa distributions. The high-energy asymptotic behavior of kappa distributions leads to a power law of the flux versus energy spectrum, while its specific formulation derives the temperature and kappa index that govern these distributions. We find that the observed temperature in most directions is about a million degrees, in agreement with most heliospheric models for the inner heliosheath. Thus, the termination shock is stronger in most places than revealed by the Voyagers' observations at their two unique crossing points. The global sky maps indicate low-temperature regions in various directions, including toward Voyager 2 where the temperature is an order of magnitude lower, consistent with in situ Voyager observations. Interestingly, the vast majority of measured kappa indices are between {approx}1.5 and {approx}2.5, consistent with the far-equilibrium 'cavity' of minimum entropy discovered by Livadiotis and McComas. The sky maps suggest that the Ribbon is a string of localized regions, while its thermodynamical behavior differentiates it from the global distributed flux. A simple model is developed to derive the density, heliosheath thickness, and thermal pressure. We find that the Ribbon thermal pressure is {approx}3.5 pDyn cm{sup -2}, roughly equal to the mechanical pressure exerted by the Local Interstellar Medium.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2011

SPECTRAL PROPERTIES OF REGIONS AND STRUCTURES IN THE INTERSTELLAR BOUNDARY EXPLORER (IBEX) SKY MAPS

We study the spectral properties of different regions and structures in the energetic neutral atom (ENA) maps at energies from {approx}0.5 keV to {approx}6 keV from the Interstellar Boundary Explorer (IBEX) mission. We find that (1) an ankle-shaped break (spectrum hardens) between {approx}1 keV and {approx}2 keV characterizes the polar spectra and the right flank, while a knee-shaped break (spectrum softens) describes the ribbon, nose, and the front region spectra; (2) the spectral indices across full latitudinal range (tail and poles) comprise a dependence reflecting a knee break at mid latitudes and an ankle break at high latitudes. This latitudinal evolution has inflection points at {approx}40 deg. S and {approx}36 deg. N, and is strongly correlated with the solar wind speed structure obtained by the Ulysses/SWOOPS instrument during its fast latitude scan in 2007. Our study confirms that the ecliptic latitude predominantly orders the spectral signatures of ENA distributions. This ordering may reflect the average solar wind properties that vary characteristically with latitude around solar minimum. We report on the spectral analyses of six regions and two structures in the IBEX maps. We also discuss the spectral asymmetries between the north and the south polar regions, their correlation with solar wind measurements, and the implications of these observations. Thus, we show detailed connections between the IBEX energy spectra and latitudinal properties of solar wind.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2011

CO-ANALYSIS OF SOLAR MICROWAVE AND HARD X-RAY SPECTRAL EVOLUTIONS. I. IN TWO FREQUENCY OR ENERGY RANGES

Solar microwave and hard X-ray spectral evolutions are co-analyzed in the 2000 June 10 and 2002 April 10 flares, and are simultaneously observed by the Owens-Valley Solar Array in the microwave band and by Yohkoh/Hard X-ray Telescope or RHESSI in the hard X-ray band, with multiple subpeaks in their light curves. The microwave and hard X-ray spectra are fitted by a power law in two frequency ranges of the optical thin part and two photon energy ranges, respectively. Similar to an earlier event in Shao and Huang, the well-known soft-hard-soft pattern of the lower energy range changed to the hard-soft-hard (HSH) pattern of the higher energy range during the spectral evolution of each subpeak in both hard X-ray flares. This energy dependence is actually supported by a positive correlation between the overall light curves and spectral evolution in the lower energy range, while it becomes an anti-correlation in the higher energy range. Regarding microwave data, the HSH pattern appears in the spectral evolution of each subpeak in the lower frequency range, which is somewhat similar to Huang and Nakajima. However, it returns back to the well-known pattern of soft-hard-harder for the overall spectral evolution in the higher frequency range of both events. This frequency dependence is confirmed by an anti-correlation between the overall light curves and spectral evolution in the lower frequency range, but it becomes a positive correlation in the higher frequency range. The possible mechanisms are discussed, respectively, for reasons why hard X-ray and microwave spectral evolutions have different patterns in different energy and frequency intervals.

74 ATOMIC AND MOLECULAR PHYSICS↗
DOE OSTI2011

SPATIALLY AND SPECTRALLY RESOLVED OBSERVATIONS OF A ZEBRA PATTERN IN A SOLAR DECIMETRIC RADIO BURST

We present the first interferometric observation of a zebra-pattern radio burst with simultaneous high spectral ({approx}1 MHz) and high time (20 ms) resolution. The Frequency-Agile Solar Radiotelescope Subsystem Testbed (FST) and the Owens Valley Solar Array (OVSA) were used in parallel to observe the X1.5 flare on 2006 December 14. By using OVSA to calibrate the FST, the source position of the zebra pattern can be located on the solar disk. With the help of multi-wavelength observations and a nonlinear force-free field extrapolation, the zebra source is explored in relation to the magnetic field configuration. New constraints are placed on the source size and position as a function of frequency and time. We conclude that the zebra burst is consistent with a double-plasma resonance model in which the radio emission occurs in resonance layers where the upper-hybrid frequency is harmonically related to the electron cyclotron frequency in a coronal magnetic loop.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2011

MODULATION OF THE GALACTIC LOW-ENERGY PROTON SPECTRUM IN THE INNER HELIOSPHERE

We study the energy spectra of 0.3-100 MeV protons and find that, at the lower part of the galactic particle spectrum, they are significantly steeper than the J(E) {approx} E spectrum predicted by analytical approximations, such as the force-field model of modulation. We select a series of low-flux periods, and approximate the spectral form by J(E) = AE{sup -{gamma}} + CE{sup {nu}}, where the two terms describe solar/heliospheric and galactic components, respectively. By determining the best fit parameters to energy spectra, correlations are sought with solar activity indices and between the parameters themselves. In the majority of cases, {nu} turns out to be between 1.2 and 1.4, with an average of 1.32 {+-} 0.12, significantly greater than the commonly expected {nu} = 1 predicted by the force-field approximation. In modulation theories {nu} > 1 corresponds to a negative Compton-Getting factor, which poses a challenge. Such an inversion may occur if the radial diffusion coefficient {kappa}{sub rr} < rV (where r is heliocentric distance and V solar wind speed), in which case a large fraction of the 10-100 MeV protons reaching 1 AU would have been cooled down within 1 AU and subsequently convected outward by the solar wind. We also find that the position of the intensity minimum of the proton spectrum dividing the solar and galactic populations shifts toward higher values with increasing solar activity. Correlations obtained with solar activity indicate that the slope of the solar/heliospheric spectrum is practically independent of solar activity. Observations are compared with numerical solutions of the modulation equation adopting simple spherical models. Possible interpretations are discussed.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2011

ANATOMY OF A SOLAR FLARE: MEASUREMENTS OF THE 2006 DECEMBER 14 X-CLASS FLARE WITH GONG, HINODE, AND RHESSI

Some of the most challenging observations to explain in the context of existing flare models are those related to the lower atmosphere and below the solar surface. Such observations, including changes in the photospheric magnetic field and seismic emission, indicate the poorly understood connections between energy release in the corona and its impact in the photosphere and the solar interior. Using data from Hinode, TRACE, RHESSI, and GONG we study the temporal and spatial evolution of the 2006 December 14 X-class flare in the chromosphere, photosphere, and the solar interior. We investigate the connections between the emission at various atmospheric depths, including acoustic signatures obtained by time-distance and holography methods from the GONG data. We report the horizontal displacements observed in the photosphere linked to the timing and locations of the acoustic signatures we believe to be associated with this flare, their vertical and horizontal displacement velocities, and their potential implications for current models of flare dynamics.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2010

A TORSIONAL ALFVEN WAVE EMBEDDED WITHIN A SMALL MAGNETIC FLUX ROPE IN THE SOLAR WIND

We describe and use novel techniques to analyze a striking and distinct solar wind event observed by two spacecraft. We show that the event is consistent with an interpretation as a torsional Alfven wave embedded within a small, nearly radially aligned, magnetic flux rope of total width {approx}10{sup 6} km. It seems likely that the torsional wave was generated by distortions produced within a pre-existing flux rope that erupted from the Sun. Our examination of many events previously identified as flux ropes in the solar wind indicates that torsional Alfven waves are extremely rare in such events.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2010

ENERGETIC NEUTRAL ATOMS: AN ADDITIONAL SOURCE FOR HELIOSPHERIC PICKUP IONS

Recently, Schwadron and McComas discussed the possibility of inner source pickup particles originating from the ionization of energetic neutral atoms (ENAs), based on new data from the IBEX mission. This proposition has some interesting features, namely, it might be able to explain why inner source pickup ions (PUIs) have a composition resembling solar abundances and show no indication of overabundance of refractory elements, although this should be expected, if the conventional explanation of solar wind-dust interaction for the origin of this heliospheric component were correct. In this Letter, we explore further consequences for ENA-related PUIs and investigate their velocity distributions. We conclude that this model will not reproduce the observed velocity distributions of inner source PUIs and point out a substantial deviation in their composition. However, it seems likely that the ionization of ENAs as observed with IBEX could contribute a significant amount of heliospheric suprathermal tail ions. Some possible consequences of our investigation for heliospheric particle populations are briefly discussed.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2010

SUNRISE/IMaX OBSERVATIONS OF CONVECTIVELY DRIVEN VORTEX FLOWS IN THE SUN

We characterize the observational properties of the convectively driven vortex flows recently discovered on the quiet Sun, using magnetograms, Dopplergrams, and images obtained with the 1 m balloon-borne SUNRISE telescope. By visual inspection of time series, we find some 3.1 x 10{sup -3} vortices Mm{sup -2} minute{sup -1}, which is a factor of {approx}1.7 larger than previous estimates. The mean duration of the individual events turns out to be 7.9 minutes, with a standard deviation of 3.2 minutes. In addition, we find several events appearing at the same locations along the duration of the time series (31.6 minutes). Such recurrent vortices show up in the proper motion flow field map averaged over the time series. The typical vertical vorticities are {approx_lt}6 x 10{sup -3} s{sup -1}, which corresponds to a period of rotation of some 35 minutes. The vortices show a preferred counterclockwise sense of rotation, which we conjecture may have to do with the preferred vorticity impinged by the solar differential rotation.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2010

SUPERSONIC MAGNETIC UPFLOWS IN GRANULAR CELLS OBSERVED WITH SUNRISE/IMAX

Using the IMaX instrument on board the SUNRISE stratospheric balloon telescope, we have detected extremely shifted polarization signals around the Fe I 5250.217 A spectral line within granules in the solar photosphere. We interpret the velocities associated with these events as corresponding to supersonic and magnetic upflows. In addition, they are also related to the appearance of opposite polarities and highly inclined magnetic fields. This suggests that they are produced by the reconnection of emerging magnetic loops through granular upflows. The events occupy an average area of 0.046 arcsec{sup 2} and last for about 80 s, with larger events having longer lifetimes. These supersonic events occur at a rate of 1.3 x 10{sup -5} occurrences per second per arcsec{sup 2}.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2010

TRANSVERSE COMPONENT OF THE MAGNETIC FIELD IN THE SOLAR PHOTOSPHERE OBSERVED BY SUNRISE

We present the first observations of the transverse component of a photospheric magnetic field acquired by the imaging magnetograph SUNRISE/IMaX. Using an automated detection method, we obtain statistical properties of 4536 features with significant linear polarization signal. We obtain a rate of occurrence of 7 x 10{sup -4} s{sup -1} arcsec{sup -2}, which is 1-2 orders of magnitude larger than the values reported by previous studies. We show that these features have no characteristic size or lifetime. They appear preferentially at granule boundaries with most of them being caught in downflow lanes at some point. Only a small percentage are entirely and constantly embedded in upflows (16%) or downflows (8%).

79 ASTRONOMY AND ASTROPHYSICS↗