bluuebunny/crossref_metadata_2025 huggingface dataset:
Far-ultraviolet Spectra of Main-sequence O Stars at Extremely Low Metallicity
Authors: Telford O. Grace , Chisholm John , McQuinn Kristen B. W. , Berg Danielle A.
Published: December 2021

Metal-poor massive stars dominate the light we observe from star-forming dwarf galaxies and may have produced the bulk of energetic photons that reionized the universe at high redshift. Yet, the rarity of observations of individual O stars below the 20% solar metallicity (Z
⊙) of the Small Magellanic Cloud (SMC) hampers our ability to model the ionizing fluxes of metal-poor stellar populations. We present new Hubble Space Telescope far-ultraviolet (FUV) spectra of three O-dwarf stars in the galaxies Leo P (3% Z
⊙), Sextans A (6% Z
⊙), and WLM (14% Z
⊙). We quantify equivalent widths of photospheric metal lines and strengths of wind-sensitive features, confirming that both correlate with metallicity. We infer the stars’ fundamental properties by modeling their FUV through near-infrared spectral energy distributions and identify stars in the SMC with similar properties to each of our targets. Comparing to the FUV spectra of the SMC analogs suggests that (1) the star in WLM has an SMC-like metallicity, and (2) the most metal-poor star in Leo P is driving a much weaker stellar wind than its SMC counterparts. We measure projected rotation speeds and find that the two most metal-poor stars have high

v

sin

(
i
)

≥ 290 km s−1, and estimate just a 3%–6% probability of finding two fast rotators if the metal-poor stars are drawn from the same

v

sin

(
i
)

distribution observed for O dwarfs in the SMC. These observations suggest that models should include the impact of rotation and weak winds on ionizing flux to accurately interpret observations of metal-poor galaxies in both the near and distant universe.
Cosmic Evolution of Barred Galaxies up to z ∼ 0.84
Authors: Kim Taehyun , Athanassoula E. , Sheth Kartik , Bosma Albert , Park Myeong-Gu , Lee Yun Hee , Ann Hong Bae
Published: December 2021

We explore the cosmic evolution of the bar length, strength, and light deficit around the bar for 379 barred galaxies at 0.2 < z ≤ 0.835 using F814W images from the COSMOS survey. Our sample covers galaxies with stellar masses

10.0
≤
log
(

M

*

/

M

⊙

)
≤
11.4

and various Hubble types. The bar length is strongly related to the galaxy mass, the disk scale length (h), R
50, and R
90, where the last two are the radii containing 50% and 90% of total stellar mass, respectively. Bar length remains almost constant, suggesting little or no evolution in bar length over the last 7 Gyr. The normalized bar lengths (R
bar/h, R
bar/R
50, and R
bar/R
90) do not show any clear cosmic evolution. Also, the bar strength (A
2 and Q

b
) and the light deficit around the bar reveal little or no cosmic evolution. The constancy of the normalized bar lengths over cosmic time implies that the evolution of bars and of disks is strongly linked over all times. We discuss our results in the framework of predictions from numerical simulations. We conclude there is no strong disagreement between our results and up-to-date simulations.
Tracking the Source of Solar Type II Bursts through Comparisons of Simulations and Radio Data
Authors: Hegedus Alexander M. , Manchester Ward B. , Kasper Justin C.
Published: December 2021

The most intense solar energetic particle events are produced by coronal mass ejections (CMEs) accompanied by intense type II radio bursts below 15 MHz. Understanding where these type II bursts are generated relative to an erupting CME would reveal important details of particle acceleration near the Sun, but the emission cannot be imaged on Earth due to distortion from its ionosphere. Here, a technique is introduced to identify the likely source location of the emission by comparing the dynamic spectrum observed from a single spacecraft against synthetic spectra made from hypothesized emitting regions within a magnetohydrodynamic (MHD) numerical simulation of the recreated CME. The radio-loud 2005 May 13 CME was chosen as a test case, with Wind/WAVES radio data being used to frame the inverse problem of finding the most likely progression of burst locations. An MHD recreation is used to create synthetic spectra for various hypothesized burst locations. A framework is developed to score these synthetic spectra by their similarity to the type II frequency profile derived from the Wind/WAVES data. Simulated areas with 4× enhanced entropy and elevated de Hoffmann–Teller velocities are found to produce synthetic spectra similar to spacecraft observations. A geometrical analysis suggests the eastern edge of the entropy-derived shock around (−30°, 0°) was emitting in the first hour of the event before falling off, and the western/southwestern edge of the shock centered around (6°, −12°) was a dominant area of radio emission for the 2 hr of simulation data out to 20 solar radii.
If Loud Aliens Explain Human Earliness, Quiet Aliens Are Also Rare
Authors: Hanson Robin , Martin Daniel , McCarter Calvin , Paulson Jonathan
Published: December 2021

If life on Earth had to achieve n “hard steps“ to reach humanity's level, then the chance of this event rose as time to the nth power. Integrating this over habitable star formation and planet lifetime distributions predicts >99% of advanced life appears after today, unless n < 3 and max planet duration <50 Gyr. That is, we seem early. We offer this explanation: a deadline is set by loud aliens who are born according to a hard steps power law, expand at a common rate, change their volume appearances, and prevent advanced life like us from appearing in their volumes. Quiet aliens, in contrast, are much harder to see. We fit this three-parameter model of loud aliens to data: (1) birth power from the number of hard steps seen in Earth’s history, (2) birth constant by assuming a inform distribution over our rank among loud alien birth dates, and (3) expansion speed from our not seeing alien volumes in our sky. We estimate that loud alien civilizations now control 40%–50% of universe volume, each will later control ∼ 105–3 × 107 galaxies, and we could meet them in ∼200 Myr–2 Gyr. If loud aliens arise from quiet ones, a depressingly low transition chance (<∼10−4 ) is required to expect that even one other quiet alien civilization has ever been active in our galaxy. Which seems to be bad news for the Search for Extraterrestrial Intelligence. But perhaps alien volume appearances are subtle, and their expansion speed lower, in which case we predict many long circular arcs to find in our sky.
Acoustic Wave Properties in Footpoints of Coronal Loops in 3D MHD Simulations
Authors: Riedl Julia M. , Van Doorsselaere Tom , Reale Fabio , Goossens Marcel , Petralia Antonino , Pagano Paolo
Published: December 2021

Acoustic waves excited in the photosphere and below might play an integral part in the heating of the solar chromosphere and corona. However, it is yet not fully clear how much of the initially acoustic wave flux reaches the corona and in what form. We investigate the wave propagation, damping, transmission, and conversion in the lower layers of the solar atmosphere using 3D numerical MHD simulations. A model of a gravitationally stratified expanding straight coronal loop, stretching from photosphere to photosphere, is perturbed at one footpoint by an acoustic driver with a period of 370 s. For this period, acoustic cutoff regions are present below the transition region (TR). About 2% of the initial energy from the driver reaches the corona. The shape of the cutoff regions and the height of the TR show a highly dynamic behavior. Taking only the driven waves into account, the waves have a propagating nature below and above the cutoff region, but are standing and evanescent within the cutoff region. Studying the driven waves together with the background motions in the model reveals standing waves between the cutoff region and the TR. These standing waves cause an oscillation of the TR height. In addition, fast or leaky sausage body-like waves might have been excited close to the base of the loop. These waves then possibly convert to fast or leaky sausage surface-like waves at the top of the main cutoff region, followed by a conversion to slow sausage body-like waves around the TR.
Wide Dust Gaps in Protoplanetary Disks Induced by Eccentric Planets: A Mass-eccentricity Degeneracy
Authors: Chen 陈 Yi-Xian 逸贤 , Wang 王 Zhuoxiao 卓骁 , Li 李 Ya-Ping 亚平 , Baruteau Clément , Lin 林 Douglas N. C. 潮
Published: December 2021

The tidal perturbation of embedded protoplanets on their natal disks has been widely attributed to be the cause of gap-ring structures in submillimeter images of protoplanetary disks around T Tauri stars. Numerical simulations of this process have been used to propose scaling of characteristic dust-gap width/gap-ring distance with respect to planet mass. Applying such scaling to analyze observed gap samples yields a continuous mass distribution for a rich population of hypothetical planets in the range of several Earth to Jupiter masses. In contrast, the conventional core-accretion scenario of planet formation predicts a bimodal mass function due to (1) the onset of runaway gas accretion above ∼20 Earth masses and (2) suppression of accretion induced by gap opening. Here, we examine the dust disk response to the tidal perturbation of eccentric planets as a possible resolution of this paradox. Based on simulated gas and dust distributions, we show the gap-ring separation of Neptune-mass planets with small eccentricities might become comparable to that induced by Saturn-mass planets on circular orbits. This degeneracy may obliterate the discrepancy between the theoretical bimodal mass distribution and the observed continuous gap width distribution. Despite damping due to planet–disk interaction, modest eccentricity may be sustained either in the outer regions of relatively thick disks or through resonant excitation among multiple super Earths. Moreover, the ring-like dust distribution induced by planets with small eccentricities is axisymmetric even in low viscosity environments, consistent with the paucity of vortices in Atacama Large Millimeter/submillimeter Array images.
The Dependence of the Fraction of Radio Luminous Quasars on Redshift and its Theoretical Implications
Authors: Rusinek-Abarca Katarzyna , Sikora Marek
Published: December 2021

While radio emission in quasars can be contributed to by a variety of processes (involving star-forming regions, accretion disk coronas and winds, and jets), the powering of the radio loudest quasars must involve very strong jets, presumably launched by the Blandford–Znajek mechanism incorporating the magnetically arrested disk (MAD) scenario. We focus on the latter and investigate the dependence of their fraction on redshift. We also examine the dependence of the radio-loud fraction (RLF) on BH mass (M
BH) and Eddington ratio (λ
Edd), while excluding the redshift bias by narrowing its range. In both of these investigations, we remove the bias associated with: (1) the diversity of source selection by constructing two well-defined, homogeneous samples of quasars (first within 0.7 ≤ z ≤ 1.9, second within 0.5 ≤ z ≤ 0.7); and (2) a strong drop in the RLF of quasars at smaller BH masses by choosing those with BH masses larger than 108.5
M
⊙. We confirm some of the previous results showing the increase in the fraction of radio-loud quasars with cosmic time and that this trend can be even steeper if we account for the bias introduced by the dependence of the RLF on BH mass, whereas the bias introduced by the dependence of the RLF on Eddington ratio is shown to be negligible. Assuming that quasar activities are triggered by galaxy mergers, we argue that such an increase can result from the slower drop with cosmic time of mixed mergers than of wet mergers.
Radio Morphology of Red Geysers
Authors: Roy Namrata , Moravec Emily , Bundy Kevin , Hardcastle Martin J. , Gürkan Gülay , Diego Baldi Ranieri , Leslie Sarah K. , Masters Karen , Gelfand Joseph , Riffel Rogerio , Riffel Rogemar A. , Mingo Fernandez Beatriz , Drabent Alexander
Published: December 2021

We present 150 MHz, 1.4 GHz, and 3 GHz radio imaging (LoTSS, FIRST, and VLASS) and spatially resolved ionized gas characteristics (SDSS IV-MaNGA) for 140 local (z < 0.1) early-type red geyser galaxies. These galaxies have a low star formation activity (with a star formation rate, SFR, ∼ 0.01 M
⊙ yr−1), but show unique extended patterns in spatially resolved emission-line maps that have been interpreted as large-scale ionized winds driven by active galactic nuclei (AGN). In this work, we confirm that red geysers host low-luminosity radio sources (L
1.4GHz ∼ 1022
WHz
−1). Out of 42 radio-detected red geysers, 32 are spatially resolved in LoTSS and FIRST, with radio sizes varying between ∼5–25 kpc. Three sources have radio sizes exceeding 40 kpc. A majority display a compact radio morphology and are consistent with either low-power compact radio sources (FR0 galaxies) or radio-quiet quasars. They may be powered by small-scale AGN-driven jets that remain unresolved at the current 5″ resolution of radio data. The extended radio sources, not belonging to the “compact” morphological class, exhibit steeper spectra with a median spectral index of −0.67, indicating the dominance of lobed components. The red geysers hosting extended radio sources also have the lowest specific SFRs, suggesting they either have a greater impact on the surrounding interstellar medium or are found in more massive halos on average. The degree of alignment of the ionized wind cone and the extended radio features are either 0° or 90°, indicating possible interaction between the interstellar medium and the central radio AGN.
Molecular Gas in the Nuclear Region of NGC 6240
Authors: Fyhrie Adalyn , Glenn Jason , Rangwala Naseem , Wheeler Jordan , Beck Sara , Bally John
Published: December 2021

NGC 6240 is a luminous infrared galaxy in the local universe in the midst of a major merger. We analyze high-resolution interferometric observations of warm molecular gas using CO J = 3–2 and 6–5 in the central few kpc of NGC 6240 taken by the Atacama Large Millimeter Array. Using these CO line observations, we model the density distribution and kinematics of the molecular gas between the nuclei of the galaxies. Our models suggest that a disk model represents the data poorly. Instead, we argue that the observations are consistent with a tidal bridge between the two nuclei. We also observe high-velocity redshifted gas that is not captured by the model. These findings shed light on small-scale processes that can affect galaxy evolution and the corresponding star formation.
SDSS J1059+4251, a Highly Magnified z ∼ 2.8 Star-forming Galaxy: ESI Observations of the Rest-frame UV Spectrum
Authors: Citro Annalisa , Erb Dawn K. , Pettini Max , Auger Matthew W. , Becker George D. , James Bethan L.
Published: December 2021

Detailed analyses of high-redshift galaxies are challenging because these galaxies are faint, but this difficulty can be overcome with gravitational lensing, in which the magnification of the flux enables spectroscopy with a high signal-to-noise ratio (S/N). We present the rest-frame ultraviolet (UV) Keck Echellette Spectrograph and Imager (ESI) spectrum of the newly discovered z = 2.79 lensed galaxy SDSS J1059+4251. With an observed magnitude F814W = 18.8 and a magnification factor μ = 31 ± 3, J1059+4251 is both highly magnified and intrinsically luminous, about two magnitudes brighter than

M

UV

*

at z ∼ 2–3. With a stellar mass M
* = (3.22 ± 0.20) × 1010
M
⊙, star formation rate SFR = 50 ± 7 M⊙ yr−1, and stellar metallicity Z
* ≃ 0.15–0.5 Z
⊙, J1059+4251 is typical of bright star-forming galaxies at similar redshifts. Thanks to the high S/N and the spectral resolution of the ESI spectrum, we are able to separate the interstellar and stellar features and derive properties that would be inaccessible without the aid of the lensing. We find evidence of a gas outflow with speeds up to −1000 km s−1, and of an inflow that is probably due to accreting material seen along a favorable line of sight. We measure relative elemental abundances from the interstellar absorption lines and find that α-capture elements are overabundant compared to iron-peak elements, suggestive of rapid star formation. However, this trend may also be affected by dust depletion. Thanks to the high data quality, our results represent a reliable step forward in the characterization of typical galaxies at early cosmic epochs.
Solar Wind ∼0.15–1.5 keV Electrons around Corotating Interaction Regions at 1 au
Authors: Tao Jiawei , Wang Linghua , Li Gang , Wimmer-Schweingruber Robert F. , Salem Chadi , Jian Lan K. , Bale Stuart D.
Published: December 2021

Here we present a statistical study of the ∼0.15–1.5 keV suprathermal electrons observed in uncompressed/compressed slow and fast solar wind around 59 corotating interaction regions (CIRs) with good measurements by Wind 3DP from 1995 through 1997. For each of these CIRs, we fit the strahl and halo energy spectra at ∼0.15–1.5 keV to a Kappa function with a Kappa index κ and kinetic temperature T
eff. We find that the ∼0.15–1.5 keV strahl electrons behave similarly in both slow and fast wind: the strahl number density n

s
positively correlates with the solar wind electron temperature T

e
and interplanetary magnetic field magnitude ∣B∣, while the strahl pitch angle width Θ
s
decreases with the solar wind speed V
sw. These suggest that the strahl electrons are generated by a similar/same process at the Sun in both slow and fast wind that produces these correlations, and the scattering efficiency of strahl in the interplanetary medium (IPM) decreases with V
sw. The ∼0.15–1.5 keV halo electrons also behave similarly in both slow and fast wind: the halo parameter positively correlates with the corresponding strahl parameter, and the halo number density n

h
positively correlates only with T

e
. These indicate that the halo formation process in the IPM retains most of the strahl properties, but it erases the relationship between n

s
and ∣B∣. In addition, κ in compressed wind distributes similarly to that in uncompressed wind, for both the strahl and halo. It shows that CIRs at 1 au are not a significant/effective acceleration source for the strahl and halo.
Global Non-ideal Magnetohydrodynamic Simulations of Protoplanetary Disks with Outer Truncation
Authors: Yang Haifeng , Bai Xue-Ning
Published: December 2021

It has recently been established that the evolution of protoplanetary disks is primarily driven by magnetized disk winds, requiring a large-scale magnetic flux threading the disks. The size of such disks is expected to shrink with time, as opposed to the conventional scenario of viscous expansion. We present the first global 2D non-ideal magnetohydrodynamic simulations of protoplanetary disks that are truncated in the outer radius, aiming to understand the interaction of the disk with the interstellar environment, as well as the global evolution of the disk and magnetic flux. We find that as the system relaxes, the poloidal magnetic field threading the disk beyond the truncation radius collapses toward the midplane, leading to a rapid reconnection. This process removes a substantial amount of magnetic flux from the system and forms closed poloidal magnetic flux loops encircling the outer disk in quasi-steady state. These magnetic flux loops can drive expansion beyond the truncation radius, corresponding to substantial mass loss through a magnetized disk outflow beyond the truncation radius analogous to a combination of viscous spreading and external photoevaporation. The magnetic flux loops gradually shrink over time, the rates of which depend on the level of disk magnetization and the external environment, which eventually governs the long-term disk evolution.
Globular Clusters and Streaming Velocities: Testing the New Formation Channel in High-resolution Cosmological Simulations
Authors: Schauer Anna T. P. , Bromm Volker , Boylan-Kolchin Michael , Glover Simon C. O. , Klessen Ralf S.
Published: December 2021

The formation of globular clusters and their relation to the distribution of dark matter have long puzzled astronomers. One of the most recently proposed globular cluster formation channels ties ancient star clusters to the large-scale streaming velocity of baryons relative to dark matter in the early universe. These streaming velocities affect the global infall of baryons into dark matter halos, the high-redshift halo mass function, and the earliest generations of stars. In some cases, streaming velocities may result in dense regions of dark matter-free gas that becomes Jeans unstable, potentially leading to the formation of compact star clusters. We investigate this hypothesis using cosmological hydrodynamical simulations that include a full chemical network and the formation and destruction of H2, a process crucial for the formation of the first stars. We find that high-density gas in regions with significant streaming velocities is indeed somewhat offset from the centers of dark matter halos, but this offset is typically significantly smaller than the virial radius. Gas outside of dark matter halos never reaches Jeans-unstable densities in our simulations. We postulate that low-level (Z ≈ 10−3
Z
⊙) metal enrichment by Population III supernovae may enable cooling in the extra-virial regions, allowing gas outside of dark matter halos to cool to the cosmic microwave background temperature and become Jeans unstable. Follow-up simulations that include both streaming velocities and metal enrichment by Population III supernovae are needed to understand if streaming velocities provide one path for the formation of globular clusters in the early universe.
Filament Eruption Driving EUV Loop Contraction and Then Expansion above a Stable Filament
Authors: Chandra Ramesh , Démoulin Pascal , Devi Pooja , Joshi Reetika , Schmieder Brigitte
Published: December 2021

We analyze the observations of EUV loop evolution associated with the filament eruption located at the border of an active region (AR). The event SOL2013-03-16T14:00 was observed with a large difference in view point by the Solar Dynamics Observatory and Solar Terrestrial Relations Observatory. The filament height is fitted with the sum of a linear and exponential function. These two phases point to different physical mechanisms such as tether-cutting reconnection and a magnetic instability. While no X-ray emission is reported, this event presents classical eruption features like separation of double ribbons and the growth of flare loops. We report the migration of the southern foot of the erupting filament flux rope due to the interchange reconnection with encountered magnetic loops of a neighboring AR. Parallel to the erupting filament, a stable filament remains in the core of the AR. The specificity of this eruption is that coronal loops, located above the nearly joining ends of the two filaments, first contract in phase, then expand and reach a new stable configuration close to the one present at the eruption onset. Both contraction and expansion phases last around 20 minutes. The main difference with previous cases is that the PIL bent about 180° around the end of the erupting filament because the magnetic configuration is at least tripolar. These observations are challenging for models that interpreted previous cases of loop contraction within a bipolar configuration. New simulations are required to broaden the complexity of the configurations studied.
The Detection of a Hot Molecular Core in the Extreme Outer Galaxy
Authors: Shimonishi Takashi , Izumi Natsuko , Furuya Kenji , Yasui Chikako
Published: December 2021

Interstellar chemistry in low-metallicity environments is crucial to understand chemical processes in the past metal-poor universe. Recent studies of interstellar molecules in nearby low-metallicity galaxies have suggested that metallicity has a significant effect on the chemistry of star-forming cores. Here we report the first detection of a hot molecular core in the extreme outer Galaxy, which is an excellent laboratory to study star formation and the interstellar medium in a Galactic low-metallicity environment. The target star-forming region, WB 89–789, is located at a galactocentric distance of 19 kpc. Our Atacama Large Millimeter/submillimeter Array observations in 241–246, 256–261, 337–341, and 349–353 GHz have detected a variety of carbon-, oxygen-, nitrogen-, sulfur-, and silicon-bearing species, including complex organic molecules (COMs) containing up to nine atoms, toward a warm (>100 K) and compact (<0.03 pc) region associated with a protostar (∼8 × 103
L
☉). Deuterated species such as HDO, HDCO, D2CO, and CH2DOH are also detected. A comparison of fractional abundances of COMs relative to CH3OH between the outer Galactic hot core and an inner Galactic counterpart shows a remarkable similarity. On the other hand, the molecular abundances in the present source do not resemble those of low-metallicity hot cores in the Large Magellanic Cloud. The results suggest that great molecular complexity exists even in the primordial environment of the extreme outer Galaxy. The detection of another embedded protostar associated with high-velocity SiO outflows is also reported.
The Two-step Forbush Decrease: A Tale of Two Substructures Modulating Galactic Cosmic Rays within Coronal Mass Ejections
Authors: Janvier Miho , Démoulin Pascal , Guo Jingnan , Dasso Sergio , Regnault Florian , Topsi-Moutesidou Sofia , Gutierrez Christian , Perri Barbara
Published: December 2021

Interplanetary coronal mass ejections (ICMEs) are known to modify the structure of the solar wind as well as interact with the space environment of planetary systems. Their large magnetic structures have been shown to interact with galactic cosmic rays (GCRs), leading to the Forbush decrease (FD) phenomenon. We revisit in the present article the 17 yr of Advanced Composition Explorer spacecraft ICME detection along with two neutron monitors (McMurdo and Oulu) with a superposed epoch analysis to further analyze the role of the magnetic ejecta in driving FDs. We investigate in the following the role of the sheath and the magnetic ejecta in driving FDs, and we further show that for ICMEs without a sheath, a magnetic ejecta only is able to drive significant FDs of comparable intensities. Furthermore, a comparison of samples with and without a sheath with similar speed profiles enable us to show that the magnetic field intensity, rather than its fluctuations, is the main driver for the FD. Finally, the recovery phase of the FD for isolated magnetic ejecta shows an anisotropy in the level of the GCRs. We relate this finding at 1 au to the gradient of the GCR flux found at different heliospheric distances from several interplanetary missions.
A Turbulent Heliosheath Driven by the Rayleigh–Taylor Instability
Authors: Opher M. , Drake J. F. , Zank G. , Powell E. , Shelley W. , Kornbleuth M. , Florinski V. , Izmodenov V. , Giacalone J. , Fuselier S. , Dialynas K. , Loeb A. , Richardson J.
Published: December 2021

The heliosphere is the bubble formed by the solar wind as it interacts with the interstellar medium (ISM). The collimation of the heliosheath (HS) flows by the solar magnetic field in the heliotail into distinct north and south columns (jets) is seen in recent global simulations of the heliosphere. However, there is disagreement between the models about how far downtail the two-lobe feature persists and whether the ambient ISM penetrates into the region between the two lobes. Magnetohydrodynamic simulations show that these heliospheric jets become unstable as they move down the heliotail and drive large-scale turbulence. However, the mechanism that produces this turbulence had not been identified. Here we show that the driver of the turbulence is the Rayleigh–Taylor (RT) instability produced by the interaction of neutral H atoms streaming from the ISM with the ionized matter in the HS. The drag between the neutral and ionized matter acts as an effective gravity, which causes an RT instability to develop along the axis of the HS magnetic field. A density gradient exists perpendicular to this axis due to the confinement of the solar wind by the solar magnetic field. The characteristic timescale of the instability depends on the neutral H density in the ISM and for typical values the growth rate is ∼3 years. The instability destroys the coherence of the heliospheric jets and magnetic reconnection ensues, allowing ISM material to penetrate the heliospheric tail. Signatures of this instability should be observable in Energetic Neutral Atom maps from future missions such as the Interstellar Mapping and Acceleration Probe (IMAP). The turbulence driven by the instability is macroscopic and potentially has important implications for particle acceleration.
A Powerful e
± Outflow Driven by a Proto-strange Quark Star
Authors: Li Shao-Ze , Yu Yun-Wei , Gao He , Dai Zi-Gao , Zheng Xiao-Ping
Published: December 2021

An electron–positron layer can cover the surface of a bare strange star (SS), the electric field in which can excite the vacuum and drive a pair wind by taking away the heat of the star. In order to investigate the pair-emission ability of a proto-SS, we establish a toy model to describe its early thermal evolution, where the initial trapping of neutrinos is specially taken into account. It is found that the early cooling of the SS is dominated by the neutrino diffusion rather than the conventional Urca processes, which leads to the appearance of an initial temperature plateau. During this plateau phase, the surface e
± pair emission can maintain a constant luminosity of 1048 − 1050erg s−1 for about a few to a few tens of seconds, which is dependent on the value of the initial temperature. The total energy released through this e
± wind can reach as high as ∼1051 erg. In principle, this pair wind could be responsible for the prompt emission or extended emission of some gamma-ray bursts.
Photodesorption of Acetonitrile CH3CN in UV-irradiated Regions of the Interstellar Medium: Experimental Evidence
Authors: Basalgète Romain , Ocaña Antonio Jesus , Féraud Géraldine , Romanzin Claire , Philippe Laurent , Michaut Xavier , Fillion Jean-Hugues , Bertin Mathieu
Published: December 2021

Pure acetonitrile (CH3CN) and mixed CO:CH3CN and H2O:CH3CN ices have been irradiated at 15 K with vacuum ultraviolet (VUV) photons in the 7–13.6 eV range using synchrotron radiation. VUV photodesorption yields of CH3CN and of photoproducts have been derived as a function of the incident photon energy. The coadsorption of CH3CN with CO and H2O molecules, which are expected to be among the main constituents of interstellar ices, is found to have no significant influence on the VUV photodesorption spectra of CH3CN, CHCN•, HCN, CN•, and CH3•. Contrary to what has generally been evidenced for most of the condensed molecules, these findings point toward a desorption process for which the CH3CN molecule that absorbs the VUV photon is the one desorbing. It can be ejected in the gas phase as intact CH3CN or in the form of its photodissociation fragments. Astrophysical VUV photodesorption yields, applicable to different locations, are derived and can be incorporated into astrochemical modeling. They vary from 0.67(± 0.33) × 10−5 to 2.0(± 1.0) × 10−5 molecule photon−1 for CH3CN depending on the region considered, which is high compared to other organic molecules such as methanol. These results could explain the multiple detections of gas-phase CH3CN in different regions of the interstellar medium and are well correlated to astrophysical observations of the Horsehead nebula and of protoplanetary disks (such as TW Hya and HD 163296).
Interaction between Multiple Current Sheets and a Shock Wave: 2D Hybrid Kinetic Simulations
Authors: Nakanotani M. , Zank G. P. , Zhao L.-L.
Published: December 2021

Particle acceleration behind a shock wave due to interactions between magnetic islands in the heliosphere has attracted attention in recent years. The downstream acceleration may yield a continuous increase of particle flux downstream of the shock wave. Although it is not obvious how the downstream magnetic islands are produced, it has been suggested that current sheets are involved in the generation of magnetic islands due to their interaction with a shock wave. We perform 2D hybrid kinetic simulations to investigate the interaction between multiple current sheets and a shock wave. In the simulation, current sheets are compressed by the shock wave and a tearing instability develops at the compressed current sheets downstream of the shock. As the result of this instability, the electromagnetic fields become turbulent and magnetic islands form well downstream of the shock wave. We find a “post-cursor” region in which the downstream flow speed normal to the shock wave in the downstream rest frame is decelerated to ∼ 1V
A immediately behind the shock wave, where V
A is the upstream Alfvén speed. The flow speed then gradually decelerates to 0 accompanied by the development of the tearing instability. We also observe an efficient production of energetic particles above 100 E
0 during the development of the instability some distance downstream of the shock wave, where

E

0

=

m

p

V

A

2

and m

p
is the proton mass. This feature corresponds to Voyager observations showing that the anomalous cosmic-ray intensity increase begins some distance downstream of the heliospheric termination shock.
The HASHTAG Project: The First Submillimeter Images of the Andromeda Galaxy from the Ground
Authors: Smith Matthew W. L. , Eales Stephen A. , Williams Thomas G. , Lee Bumhyun , Li Zongnan , Barmby Pauline , Bureau Martin , Chapman Scott , Cho Brian S. , Chung Aeree , Chung Eun Jung , Chung Hui-Hsuan , Clark Christopher J. R. , Clements David L. , Davis Timothy A. , De Looze Ilse , Eden David J. , Athikkat-Eknath Gayathri , Ford George P. , Gao Yu , Gear Walter , Gomez Haley L. , de Grijs Richard , He Jinhua , Ho Luis C. , Hughes Thomas M. , Jiao Sihan , Li Zhiyuan , Kemper Francisca , Kirchschlager Florian , Koch Eric W. , Kong Albert K. H. , Lee Chien-Hsiu , Lin En-Tzu , Mairs Steve , Michałowski Michał J. , Pattle Kate , Peng Yingjie , Ragan Sarah E. , Rawlings Mark G. , Rigopoulou Dimitra , Saintonge Amelie , Schruba Andreas , Tang Xindi , Wang Junfeng , Whitworth Anthony P. , Wilson Christine D. , Yim Kijeong , Zhu Ming
Published: December 2021

Observing nearby galaxies with submillimeter telescopes on the ground has two major challenges. First, the brightness is significantly reduced at long submillimeter wavelengths compared to the brightness at the peak of the dust emission. Second, it is necessary to use a high-pass spatial filter to remove atmospheric noise on large angular scales, which has the unwelcome side effect of also removing the galaxy’s large-scale structure. We have developed a technique for producing high-resolution submillimeter images of galaxies of large angular size by using the telescope on the ground to determine the small-scale structure (the large Fourier components) and a space telescope (Herschel or Planck) to determine the large-scale structure (the small Fourier components). Using this technique, we are carrying out the HARP and SCUBA-2 High Resolution Terahertz Andromeda Galaxy Survey (HASHTAG), an international Large Program on the James Clerk Maxwell Telescope, with one aim being to produce the first high-fidelity high-resolution submillimeter images of Andromeda. In this paper, we describe the survey, the method we have developed for combining the space-based and ground-based data, and we present the first HASHTAG images of Andromeda at 450 and 850 μm. We also have created a method to predict the CO(J = 3–2) line flux across M31, which contaminates the 850 μm band. We find that while normally the contamination is below our sensitivity limit, it can be significant (up to 28%) in a few of the brightest regions of the 10 kpc ring. We therefore also provide images with the predicted line emission removed.
Classical Novae at Radio Wavelengths
Authors: Chomiuk Laura , Linford Justin D. , Aydi Elias , Bannister Keith W. , Krauss Miriam I. , Mioduszewski Amy J. , Mukai Koji , Nelson Thomas J. , Rupen Michael P. , Ryder Stuart D. , Sokoloski Jennifer L. , Sokolovsky Kirill V. , Strader Jay , Filipović Miroslav D. , Finzell Tom , Kawash Adam , Kool Erik C. , Metzger Brian D. , Nyamai Miriam M. , Ribeiro Valério A. R. M. , Roy Nirupam , Urquhart Ryan , Weston Jennifer
Published: December 2021

We present radio observations (1–40 GHz) for 36 classical novae, representing data from over five decades compiled from the literature, telescope archives, and our own programs. Our targets display a striking diversity in their optical parameters (e.g., spanning optical fading timescales, t
2 = 1–263 days), and we find a similar diversity in the radio light curves. Using a brightness temperature analysis, we find that radio emission from novae is a mixture of thermal and synchrotron emission, with nonthermal emission observed at earlier times. We identify high brightness temperature emission (T

B
> 5 × 104 K) as an indication of synchrotron emission in at least nine (25%) of the novae. We find a class of synchrotron-dominated novae with mildly evolved companions, exemplified by V5589 Sgr and V392 Per, that appear to be a bridge between classical novae with dwarf companions and symbiotic binaries with giant companions. Four of the novae in our sample have two distinct radio maxima (the first dominated by synchrotron and the later by thermal emission), and in four cases the early synchrotron peak is temporally coincident with a dramatic dip in the optical light curve, hinting at a common site for particle acceleration and dust formation. We publish the light curves in a machine-readable table and encourage the use of these data by the broader community in multiwavelength studies and modeling efforts.
MAVEN Observations of Periodic Low-altitude Plasma Clouds at Mars
Authors: Zhang Chi , Rong Zhaojin , Nilsson Hans , Klinger Lucy , Xu Shaosui , Futaana Yoshifumi , Wei Yong , Zhong Jun , Fränz Markus , Li Kun , Zhang Hui , Fan Kai , Wang Lei , Holmström Mats , Ge Yasong , Cui Jun
Published: December 2021

Ion escape to space through the interaction of solar wind and Mars is an important factor influencing the evolution of the Martian atmosphere. The plasma clouds (explosive bulk plasma escape), considered an important ion escaping channel, have been recently identified by spacecraft observations. However, our knowledge about Martian plasma clouds is lacking. Based on the observations of the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft, we study a sequence of periodic plasma clouds that occurred at low altitudes (∼600 km) on Mars. We find that the heavy ions in these clouds are energy-dispersed and have the same velocity, regardless of species. By tracing such energy-dispersed ions, we find the source of these clouds is located in a low-altitude ionosphere (∼120 km). The average tailward moving flux of ionospheric plasma carried by clouds is on the order of 107 cm−2 s−1, which is one order higher than the average escaping flux for the magnetotail, suggesting explosive ion escape via clouds. Based on the characteristics of clouds, we suggest, similar to the outflow of Earth’s cusp, these clouds might be the product of heating due to solar wind precipitation along the open field lines, which were generated by magnetic reconnection between the interplanetary magnetic field and crustal fields that occurred above the source.
The Antecedents of Psychological Empowerment and Its Impact towards General Physician Job Performance
Authors: Regina Marischa , Henny Santika , Antonio Ferdi
Published: December 2021

BACKGROUND: The emergence of new infectious diseases such as SARS-CoV-2 (Coronavirus Disease 19) creates a burden to the healthcare system especially to the front liners such as medical doctors. The job performance of the general practitioners related to quality of care to SARS-CoV2 patients.
AIM: ​​The purpose of this study is to analyze the antecedents of psychological empowerment towards job performance, mediated by service orientation. These antecedents could be seen in hospital perspectives and professional life.
 
METHODS: This is a quantitative survey study using a cross-sectional approach. 185 samples purposively obtained from the general practitioners who work at SARS-CoV-2 Reference Private Hospital in Jakarta and surrounding area. Data collection using online questionnaires and analyzed by SmartPLS 3.3.3™ .
RESULTS: There are nine hypotheses that are supported in this research. The strongest predictor of psychological empowerment is the training opportunities, followed by relationships with fellow doctors and autonomy at work. Psychological empowerment has been proven to have a direct impact on job performance, while service orientation has been found as a mediation in this relationship.
CONCLUSION: Psychological empowerment has been proven as an important construct to predict job performance, therefore hospital management has to pay more attention to psychological empowerment for GPs during the pandemic. Training opportunities should be prioritized by the board of directors of the hospitals, they should allocate time and the resources to facilitate the training opportunity.
KEYWORDS: Psychological empowerment, service orientation, job performance, general practitioner, SARS-CoV-2 referral private hospital.
The Psychological Experiences of Using Islamic Philosophy Approach among Women’s with Advanced Breast Cancer in Indonesia
Authors: Komariah Maria , Qadous Shurouq Ghalib , Firdaus Mohd Khairul Zul Hasymi , Agustina Hana Rizmadewi , Mediawati Ati Surya , Yulianita Henny , Praptiwi Atlastieka , Setyorini Dyah , Permana Ryan Hara
Published: December 2021

BACKGROUND: Breast cancer turns a person’s life upside down, affecting every aspect of an individual including the psychological domain, such as feelings of phobia, isolation, anger, irritability, confusion, and most frequently anxiety. Some studies reported that rituals practice in Islam have an impact on the psychological health breast cancer patient.

AIM: The aim of the study was to explore the experience of psychological alteration among patients with advanced breast cancer.

METHODS: A qualitative study utilizing the content analysis approach was organized. Twenty Muslims with breast cancer during chemotherapy treatment with a mean age of 47.1 years who dealt with their psychological responses during treatment were invited to participate in a semi-structured interview, before and after applying Islamic-based practice therapy. This study conducted between February and June 2018 in the outpatient unit of chemotherapy in one of the Indonesia’s teaching hospitals. The generated data were transcribed verbatim and the content analysis approach was used for data reduction, data names, obtaining analytical code, and determining categories and themes.

RESULTS: Four themes emerged from the data analysis before the researchers using the Islamic-based practice therapy: (1) Self-blaming, (2) feeling sad, (3) feeling fear and uncertain, and (4) living with a new body. However, the results after applying the Islamic-based practice therapy emerged three themes: (1) Closer to God, (2) peace of mind, and (3) inner strength.

CONCLUSION: Overall, in the view of breast cancer patients, the psychological experience of using the Islamic-based practice therapy could change to positive responses by making them feel closer to God, having good inner strength, and a peaceful mind in dealing with their day-to-day conditions. Hence, understanding the patient’s experience will assist the nurses to promote professional abilities and improve nursing care delivery related to different cultural backgrounds and spiritual dimensions of Muslims patients.
L’épopée d’un exilé en quête d’asile
Authors: Momo Donaya Mitterand Mardoché , Bouseta Hanane , Sajot Florence
Published: December 2021

Cet article relate le parcours d’un exilé camerounais, Mitterand, qui pour fuir la dictature, place sa confiance chez des passeurs pour rejoindre l’Europe. Son voyage se transforme rapidement en véritable cauchemar alternant entre espoirs et désillusions. Son récit lève le voile sur les arcanes de l’exil.
Faire place aux personnes précaires. Leurs parcours d’accès aux droits et aux soins, notamment en santé mentale
Authors: Langer-Sautière Laurence , Borie Nicole , Rialle Vincent
Published: December 2021

L’ objet de l’étude est l’échec croissant de la fonction institutionnelle d’accueil et de prise en charge des personnes précaires dans leur processus d’accès aux droits et aux soins, notamment psychiques. L’ approche est celle d’une recherche-action visant l’analyse puis le dépassement des obstacles à l’écoute attentionnée de la personne, écoute préalable à toute réponse adaptée et éventuellement co-construite avec la personne ainsi accueillie. La méthode comprend d’une part l’étude de nombreux documents et rapports de travail émis au sein de l’ensemble du réseau d’accueil (secteur associatif, services municipaux, et organismes gouvernementaux liés à la précarité), d’autre part l’organisation d’un groupe de professionnels du réseau (psychologues, travailleurs sociaux, acteurs institutionnels…) avec des séances de groupe pour l’expression des difficultés rencontrées au quotidien par ces professionnels. Les résultats montrent des sentiments de désespoir, une fragmentation du travail, des injonctions administratives incompatibles avec la profession d’accueil et de conseil psychologique, un sentiment d’insécurité, etc. Une discussion situe ensuite ce travail dans un contexte et une perspective élargis. Enfin, une conclusion évoque le dépassement du seul constat d’impuissance et les perspectives d’action transformatrice des politiques publiques et de regain, chez ces professionnels, de leurs capacités de réponse et de créativité professionnelles propres.
L’équivocité de l’Eros
Authors: Deudon Aurélien
Published: December 2021

Les érotiques phénoménologiques françaises ont sans conteste contribué à libérer la conception de la sexualité humaine de la reproduction, de la génitalité et du plaisir, auxquels elle était traditionnellement réduite. Cependant, ces érotiques ont donné lieu à des descriptions du sexe sans les sexes – moins par angélisme que par androcentrisme spontané. À l’encontre de ce monosexualisme tacite, nous tentons de prolonger l’intuition de Simone de Beauvoir qui dès Le Deuxième Sexe envisage de distinguer l’éros masculin de l’éros féminin. En plus de réinvestir cette dualité de l’Eros, cet article table sur l’analyse phénoménologique des caresses érotiques pour proposer de faire droit à trois sexes existentiaux.
Le vécu parental du parcours diagnostique dans l’autisme : discussion autour d’une étude qualitative
Authors: Leblé Nicolas , Cosquer Mireille , Mezghiche Lilia , Cazard Florence , Jousselme Catherine
Published: December 2021

Le parcours de soin d’un enfant avec autisme impacte fortement l’expérience parentale. Par ailleurs, les parents sont les interlocuteurs principaux des professionnels prenant en charge ces enfants. Enfin, ces parents, à l’échelle individuelle ou collective, mènent des actions et influent sur la perception de l’autisme dans le champ social. Nous tentons d’appréhender leur vécu du parcours diagnostique et de soin de leur enfant, à partir d’une étude qualitative fondée sur des témoignages de parents ayant consulté pour une évaluation dans un Centre de Diagnostic Autisme entre 2007 et 2015. Nous décrivons certains aspects saillants de ce parcours, depuis leurs premières inquiétudes jusqu’à l’évaluation diagnostique de l’enfant, et rapportons les difficultés rencontrées ainsi que les mouvements psychiques qui s’y associent. Enfin, nous discutons ces résultats qui mettent en lumière l’impératif, pour le professionnel, d’associer les parents aux prises en charge dans une position active.