adsabs/SciX_UAT_keywords huggingface dataset:
Influence of Intermittency on the Energy Transfer Rate of Solar Wind Turbulence

The intermittency in the solar wind turbulence manifests itself in the anisotropic scaling due to the anisotropic spectral index and the intermittent level based on the extended P model. However, the influence of intermittency on the energy transfer rate remains unclear. Here we apply the partial variance of increments method to identify the intermittency for the magnetic field measurements in the fast solar wind from the Ulysses spacecraft. We distinguish the sampling direction using the angle θ RB between the local magnetic field and radial direction to study the anisotropy. We perform the multiorder structure function analyses and adopt the log-Poisson cascade model to describe the role of intermittency in the cascade process. We find that the anisotropy of the scaling becomes isotropic with a complete removal of intermittency. We compare explicitly the anisotropy of the energy transfer rate before and after removing the intermittency for the same interval for the first time. We find a distinct anisotropy with a cascade enhancement in the direction perpendicular to the local magnetic field. The removal of the intermittency greatly weakens the anisotropy by mainly reducing the perpendicular energy transfer rate. Our findings suggest that the intermittency effectively enhances the energy transfer rate, in particular in the perpendicular direction in the solar wind turbulence.

Keywords: fast solar wind; interplanetary turbulence; interplanetary magnetic fields; magnetohydrodynamics
Revisiting the Mass-excitation (MEx) Diagram using the MaNGA Data Set

The diagram comparing the flux ratio of the [O III] and Hβ emission lines with the total stellar mass of galaxies (also known as the mass-excitation diagram, MEx) has been widely used to classify the ionization mechanism in high redshift galaxies, dividing star-forming galaxies from those where active galactic nuclei are important. This diagram was mainly derived using single-fiber spectroscopy from the SDSS-DR7 survey. In this study, we revise this diagram using the central and integrated spectral measurement from the entire Integral Field Spectroscopic MaNGA sample. Our results suggest that along with these physical parameters, the equivalent width of the Hα emission line is also required to constrain the ionization mechanism of a high-redshifted galaxy. Furthermore, the location of a galaxy in the excitation-mass diagram varies depending on the use of central or integrated properties.

Keywords: high-redshift galaxies; surveys; spectroscopy; astronomical techniques; active galactic nuclei
A Fireball and Potentially Hazardous Binary Near-Earth Asteroid (164121) 2003 YT1

We present a fireball detected in the night sky over Kyoto, Japan on UT 2017 April 28 at {15}{{h}} {58}{{m}} {19}{{s}} by the SonotaCo Network. The absolute visual magnitude is {M}{{v}} = -4.10 ± 0.42 mag. Luminous light curves obtain a meteoroid mass of m = 29 ± 1 g, corresponding to the size of a s = 2.7 ± 0.1 cm. Orbital similarity assessed by D-criterions (see D SH = 0.0079) has identified a likely parent, the binary near-Earth asteroid (164121) 2003 YT1. The suggested binary formation process is a Yarkovsky-O’Keefe-Radzievskii-Paddack-driven rotational disintegration. The asynchronous state indicates the age of <104 yr, near or shorter than the upper limit to meteoroid stream lifetime. We examine potential dust production mechanisms for the asteroid, including rotational instability, resurfacing, impact, photoionization, radiation pressure sweeping, thermal fracture, and sublimation of ice. We find some of them capable of producing the meteoroid-scale particles. Rotational instability is presumed to cause mass shedding, in consideration of the recent precedents (e.g., asteroid (6478) Gault), possibly releasing millimeter-centimeter scale dust particles. Impacts by micrometeorites with a size ≃1 mm could be a trigger for ejecting the centimeter-sized particles. Radiation pressure can sweep out the millimeter-sized dust particles, while not sufficient for the centimeter-sized. The other mechanisms are unprovable or unidentified. The feasibility in the parental aspect of 2003 YT1 is somewhat reconciled with the fireball observation, yielding an insight into how we approach potentially hazardous objects.

Keywords: solar system astronomy; meteors; fireballs; asteroids; near-earth objects; meteor radiants; surveys; catalogs; micrometeoroids
Inference of the Local Interstellar Spectra of Cosmic-Ray Nuclei Z ≤ 28 with the GALPROP-HELMOD Framework

Composition and spectra of Galactic cosmic rays (CRs) are vital for studies of high-energy processes in a variety of environments and on different scales, for interpretation of γ-ray and microwave observations, for disentangling possible signatures of new phenomena, and for understanding of our local Galactic neighborhood. Since its launch, AMS-02 has delivered outstanding-quality measurements of the spectra of $\bar{p}$ , ${e}^{\pm }$ , and nuclei: 1H-8O, 10Ne, 12Mg, 14Si. These measurements resulted in a number of breakthroughs; however, spectra of heavier nuclei and especially low-abundance nuclei are not expected until later in the mission. Meanwhile, a comparison of published AMS-02 results with earlier data from HEAO-3-C2 indicates that HEAO-3-C2 data may be affected by undocumented systematic errors. Utilizing such data to compensate for the lack of AMS-02 measurements could result in significant errors. In this paper we show that a fraction of HEAO-3-C2 data match available AMS-02 measurements quite well and can be used together with Voyager 1 and ACE-CRIS data to make predictions for the local interstellar spectra (LIS) of nuclei that are not yet released by AMS-02. We are also updating our already-published LIS to provide a complete set from 1H-28Ni in the energy range from 1 MeV nucleon-1 to ∼100-500 TeV nucleon-1, thus covering 8-9 orders of magnitude in energy. Our calculations employ the GALPROP-HELMOD framework, which has proved to be a reliable tool in deriving the LIS of CR $\bar{p}$ , e-, and nuclei 1H-8O.

Keywords: galactic cosmic rays; interplanetary medium; interstellar medium; heliosphere; cosmic ray sources; cosmic ray detectors
Persistent Starspot Signals on M Dwarfs: Multiwavelength Doppler Observations with the Habitable-zone Planet Finder and Keck/HIRES

Young, rapidly rotating M dwarfs exhibit prominent starspots, which create quasiperiodic signals in their photometric and Doppler spectroscopic measurements. The periodic Doppler signals can mimic radial velocity (RV) changes expected from orbiting exoplanets. Exoplanets can be distinguished from activity-induced false positives by the chromaticity and long-term incoherence of starspot signals, but these qualities are poorly constrained for fully convective M stars. Coherent photometric starspot signals on M dwarfs may persist for hundreds of rotations, and the wavelength dependence of starspot RV signals may not be consistent between stars due to differences in their magnetic fields and active regions. We obtained precise multiwavelength RVs of four rapidly rotating M dwarfs (AD Leo, G227-22, GJ 1245B, GJ 3959) using the near-infrared (NIR) Habitable-zone Planet Finder and the optical Keck/HIRES spectrometer. Our RVs are complemented by photometry from Kepler, TESS, and the Las Cumbres Observatory network of telescopes. We found that all four stars exhibit large spot-induced Doppler signals at their rotation periods, and investigated the longevity and optical-to-NIR chromaticity for these signals. The phase curves remain coherent much longer than is typical for Sunlike stars. Their chromaticity varies, and one star (GJ 3959) exhibits optical and NIR RV modulation consistent in both phase and amplitude. In general, though, we find that the NIR amplitudes are lower than their optical counterparts. We conclude that starspot modulation for rapidly rotating M stars frequently remains coherent for hundreds of stellar rotations and gives rise to Doppler signals that, due to this coherence, may be mistaken for exoplanets.

Keywords: starspots; exoplanets; time series analysis; m dwarf stars; gaussian processes regression; radial velocity; stellar photometry; high resolution spectroscopy
Wave-polarization Analysis of the Alfvénic Slow Solar Wind at Kinetic Scales

This paper reports the first polarization measurement in the Alfvénic slow solar wind. The normalized magnetic helicity is used as a diagnostic parameter for studying the polarization status of the high-frequency magnetic fluctuations, along with an attempt to identify various wave modes in the solar wind turbulence. Clear evidence for the existence of ion cyclotron waves (ICWs) and kinetic Alfvén waves (KAWs) is also found in the Alfvénic low-speed plasma, robustly supporting the idea that the Alfvénic content of the solar wind fluctuations at fluid scales is the key parameter driving wave generation at kinetic scales. By separating the contributions to helicity from the two modes, it is possible to address the thermodynamical properties of ICWs and KAWs and provide the first direct estimate of their magnetic compressibility. In particular, while ICWs are mainly associated with higher levels of anisotropy and appear to be bounded by the threshold of proton-cyclotron kinetic instability, KAWs (which end up being more compressive than ICWs) are found at lower anisotropies and seem to be limited by the mirror mode instability threshold, extending as well to near the parallel fire hose unstable region. These result are relevant to theories of turbulence and dissipation in the solar wind.

Keywords: interplanetary turbulence; alfven waves; space plasmas; solar wind; magnetohydrodynamics
A Search for OH 18 cm Emission from Intermediate-velocity Gas at High Galactic Latitudes

We present search results of 22 high-latitude (∣b∣ > 25°) sightlines for OH 18 cm emission using the 305 m radio telescope at the Arecibo Observatory. These sightlines appear in neutral hydrogen emission at intermediate velocities -90 ≤ V LSR ≤ -20 km s-1 and are predicted to have a sufficient molecular composition so as to be detectable in molecular emission. Such objects, known as intermediate-velocity molecular clouds (IVMCs), have historically been detected through 12CO emission. Recent studies indicate that IVMCs may be widespread in the galaxy and have important implications for models of the interstellar medium and star formation. However, we report nondetections of OH emission toward the 22 sightlines and provide stringent upper limits on the OH column density. Using available H I and A v data in combination with existing state-of-the-art PDR models, we estimate H2 column densities and find that they are more than an order of magnitude lower than the predicted values. We also find that the hydrogen volume density of these clouds is ≲25 cm-3. In addition, we discuss the known IVMCs with previous 12CO detections in the context of the PDR models. Our analysis of these clouds indicates that the structure of molecular material in IVMCs is morphologically clumpy. These results motivate the need for future sensitive, on-the-fly searches (rather than targeted searches) for CO emission from IVMCs with resolutions on the order of ~1'. High angular resolution (~1') H I and A v data will also be helpful to better constrain the structure and composition of IVMCs.

Keywords: interstellar medium; interstellar clouds; diffuse interstellar clouds; interstellar molecules; radio spectroscopy; electron impact ionization
First Determination in the Extended Corona of the 2D Thermal Evolution of a Current Sheet after a Solar Eruption

For the first time the evolution of the coronal reconfiguration after a coronal mass ejection (CME) was observed by the multichannel Metis Coronagraph on board the ESA–Solar Orbiter mission. The images acquired in visible light (VL) between 3.0 and 5.4 R ⊙ show the formation after a CME of a bright elongated radial feature interpreted as a post-CME current sheet (CS). The unique combination of VL and UV images allowed the time evolution of multiple plasma physical parameters inside and outside the CS region to be mapped in 2D for the first time. The CS electron temperature reached peak values higher than 1 MK, more than twice as high as the surrounding corona. An elongated vertical diffusion region, characterized as a region of much higher thermal pressure and lower magnetic pressure, is observed to slowly propagate outward during 13 hr of observations. Inside this region the Alfvénic Mach number is of the order of M A ≃ 0.02–0.11, the plasma β is close to unity, and the level of turbulence is higher than in the surrounding corona, but decreases slowly with time. All these results provide one of the most complete pictures of these features, and support the idea of a magnetic reconnection coupled with turbulence, thus allowing significant heating of the local plasma, despite the weakness of involved coronal magnetic fields in the considered altitude range.

Keywords: active solar corona; solar coronal mass ejections; solar ultraviolet emission; coronagraphic imaging; solar corona; solar coronal transients; polarimetry; astronomy data analysis
Viscous Evolution of Magnetized Clumps: A Source for X-Ray Flares in Gamma-Ray Bursts

X-ray flares may indicate the late-time activity of the central engines of gamma-ray bursts. Such long-term activity has been described through some models, one of which is the viscous evolution of the outer disk’s fragments proposed by Perna et al., and developed quantitatively by Dall’Osso et al. Here, we reconstruct the framework of Dall’Osso et al. by taking both small- and large-scale effects of magnetic field into account. To consider the magnetic barrier as a possible mechanism that might govern the accretion process of each magnetized clump, we construct a simple pattern in boundary conditions through which this mechanism might act. Regarding various model parameters, we probe for their influence and follow some key analogies between our model predictions and previous phenomenological estimates, for two different choices of boundary conditions (with and without a magnetic barrier). Our model is remarkably capable of matching the bolometric and X-ray light curves of flares, as well as reproducing their statistical properties, such as the ratios between rise and decay time, width parameter and peak time, and the power-law correlation between peak luminosity and peak time. Combining our results with the conclusions of previous studies, we are led to interpret a magnetic barrier as a less probable mechanism that might control the evolution of these clumps, especially those created later (or viscously evolved ones).

Keywords: accretion; gamma-ray bursts; magnetic fields
A Search for Neutrino Point-source Populations in 7 yr of IceCube Data with Neutrino-count Statistics

The presence of a population of point sources in a data set modifies the underlying neutrino-count statistics from the Poisson distribution. This deviation can be exactly quantified using the non-Poissonian template fitting technique, and in this work we present the first application of this approach to the IceCube high-energy neutrino data set. Using this method, we search in 7 yr of IceCube data for point-source populations correlated with the disk of the Milky Way, the Fermi bubbles, the Schlegel, Finkbeiner, and Davis dust map, or with the isotropic extragalactic sky. No evidence for such a population is found in the data using this technique, and in the absence of a signal, we establish constraints on population models with source-count distribution functions that can be described by a power law with a single break. The derived limits can be interpreted in the context of many possible source classes. In order to enhance the flexibility of the results, we publish the full posterior from our analysis, which can be used to establish limits on specific population models that would contribute to the observed IceCube neutrino flux.

Keywords: astrostatistics; astrostatistics distributions; bayesian statistics; neutrino astronomy; high energy astrophysics; neutrino telescopes; posterior distribution
Tracing the Total Stellar Mass and Star Formation of High-redshift Protoclusters

As the progenitors of present-day galaxy clusters, protoclusters are excellent laboratories to study galaxy evolution. Since existing observations of protoclusters are limited to the detected constituent galaxies at UV and/or infrared wavelengths, the details of how typical galaxies grow in these young, pre-virialized structures remain uncertain. We measure the total stellar mass and star formation within protoclusters, including the contribution from faint undetected members by performing a stacking analysis of 211 z = 2-4 protoclusters selected as Planck cold sources. We stack Wide-field Infrared Survey Explorer and Herschel/SPIRE images to measure the angular size and the spectral energy distribution of the integrated light from the protoclusters. The fluxes of protoclusters selected as Planck cold sources can be contaminated by line-of-sight interlopers. Using the WebSky simulation, we estimate that a single protocluster contributes 33% ± 15% of the flux of a Planck cold source on average. After this correction, we obtain a total star formation rate of 7.3 ± 3.2 × 103 M ⊙yr-1 and a total stellar mass of 4.9 ± 2.2 × 1012 M ⊙. Our results indicate that protoclusters have, on average, 2× more star formation and 4× more stellar mass than the total contribution from individually detected galaxies in spectroscopically confirmed protoclusters. This suggests that much of the total flux within z = 2-4 protoclusters comes from galaxies with luminosities lower than the detection limit of SPIRE (L IR < 3 × 1012 L ⊙). Lastly, we find that protoclusters subtend a half-light radius of 2.'8 (4.2-5.8 cMpc), which is consistent with simulations.

Keywords: galaxy evolution; infrared galaxies; high-redshift galaxy clusters
A New Cold Stream near the Southern Galactic Pole

We report the discovery of a cold stream near the southern Galactic pole (dubbed as SGP-S) detected in Gaia Early Data Release 3. The stream is at a heliocentric distance of ~9.5 kpc and spans nearly 58° by 0.°6 on sky. The color-magnitude diagram of SGP-S indicates an old and metal-poor (age ~12 Gyr, [M/H] ~ -2.0 dex) stellar population. The stream's surface brightness reaches an exceedingly low level of Σ G ≃ 36.2 mag arcsec-2. Neither extant globular clusters nor other known streams are associated with SGP-S.

Keywords: milky way galaxy; milky way stellar halo; tidal tails; globular star clusters
RGS Observations of Ejecta Knots in Tycho's Supernova Remnant

We present results from XMM-Newton/Reflection Grating Spectrometer (RGS) observations of prominent knots in the southernmost portion of Tycho's supernova remnant, known to be the remnant of a Type Ia supernova in 1572 C.E. By dispersing the photons from these knots out of the remnant with very little emission in front of or behind them, we obtained the nearly uncontaminated spectra of the knots. In the southernmost knot, the RGS successfully resolved numerous emission lines from Si, Ne, O Heα and Lyα, and Fe L-shell. This is the first clear detection of O lines in Tycho's supernova remnant. Line broadening was measured to be ∼3 eV for the O Heα and ∼4.5 eV for the Fe L lines. If we attribute the broadening to pure thermal Doppler effects, then we obtain kTO and kTFe to be ∼400 keV and 1.5 MeV, respectively. These temperatures can be explained by heating in a reverse shock with a shock velocity of ∼3500 km s-1. The abundances obtained from fitting the RGS and MOS data together imply substantially elevated amounts of these materials, confirming previous studies that the knots are heated by a reverse shock, and thus contain ejecta material from the supernova. We are unable to find a Type Ia explosion model that reproduces these abundances, but this is likely the result of this knot being too small to extrapolate to the entire remnant.

Keywords: supernova remnants; shocks; plasma astrophysics; ejecta; supernovae
Spectroscopic Orbits of Subsystems in Multiple Stars. VIII.

Periods, eccentricities, and masses in hierarchical stellar systems inform us on the formation and early evolution of these fascinating objects. To complement the multiplicity statistics of nearby solar-type stars, 19 new spectroscopic orbits of inner subsystems in 15 hierarchies (10 triples and 5 quadruples) are determined based on high-resolution echelle spectra collected during several years. While previous papers of this series contained mostly short-period orbits, here most periods are on the order of a year. The main components of these hierarchies are HIP 7852, HIP 9148, HIP 12548, HIP 21079, HIP 24320, HIP 27970, HIP 34212, HIP 56282, HIP 57860, HIP 76400, HIP 76816, HIP 81394, HIP 96284, HIP 100420, and HD 108938. Noteworthy systems are HIP 12548 and HIP 24230 (hierarchies of 2+2 architecture with low-mass spectroscopic secondaries), HIP 56282 (a planetary-type 3+1 hierarchy), and HIP 27970 (a compact triple with periods of 15 and 1049 days).

Keywords: spectroscopic binary stars; visual binary stars; multiple stars
Thermally Driven Angular Momentum Transport in Hot Jupiters

We study the angular momentum transport inside hot Jupiters under the influence of gravitational and thermal forcing. Due to the strong stellar irradiation, a radiative region develops on top of the convective region. Internal gravity waves are launched at the radiative-convective boundaries (RCBs). The thermal response is dynamical and plays an important role in the angular momentum transport. By separating the gravitational and thermal forcing terms, we identify the thermal effects of increasing the angular momentum transport. For the low-frequency (in the corotating frame with planets) prograde (retrograde) tidal frequency, the angular momentum flux is positive (negative). The tidal interactions tend to drive the planet to the synchronous state. We find that the angular momentum transport associated with the internal gravity wave is very sensitive to relative position between the RCB and the penetration depth of the thermal forcing. If the RCB is in the vicinity of the thermal forcing penetration depth, even with small amplitude thermal forcing, the thermally driven angular momentum flux could be much larger than the flux induced by gravitational forcing. The thermally enhanced torque could drive the planet to the synchronous state in as short as a few 104 yr.

Keywords: internal waves; exoplanet atmospheres; exoplanet structure; hydrodynamics; exoplanet tides