bluuebunny/crossref_metadata_2025_split huggingface dataset:
Introduction
Authors: Jaywant Abhishek , Oberlin Lauren E. , Cherestal Stephanie , Bueno Castellano Christina , Wilkins Victoria M. , Kanellopoulos Dora 
Published: November 2023

Abstract
This introductory chapter explores the treatment program developed for individuals with persistent symptoms of COVID-19. Some individuals who contract COVID-19 experience persistent symptoms of the illness, even after the acute infection. Thus, the tools and techniques for the treatment program were largely drawn and adapted from psychotherapy approaches in other medical conditions and other cognitive behavioral therapy manuals. Additionally, some modules are designed to help manage cognitive difficulties, brain fog, fatigue and sleep disturbance, while some modules require rehabilitation from physical therapy, occupational therapy, and speech-language pathology from other medical professionals. The chapter provides an overview of the key components of the treatment program, such as learning how emotions affect medical symptoms and physical function.
Module 1: Setting Goals for Therapy
Authors: Jaywant Abhishek , Oberlin Lauren E. , Cherestal Stephanie , Bueno Castellano Christina , Wilkins Victoria M. , Kanellopoulos Dora 
Published: November 2023

Abstract
This chapter discusses how to work with the therapist to set goals for therapy. It highlights the importance of identifying personal goals for treatment, since goals reflect concerns, problematic symptoms, or difficulties that need to be addressed. These goals also serve as motivation for change and engagement with the treatment program. The chapter covers strategies to explore ambivalence with the therapist and increase motivation, as people often feel ambivalence or uncertainty about making changes when starting therapy. One worksheet focuses on identifying long-term goals and short-term goals, and another worksheet allows people to consider the advantages and disadvantages of making a desired change.
Module 2: Covid-19 and the Cognitive Behavioral Model
Authors: Jaywant Abhishek , Oberlin Lauren E. , Cherestal Stephanie , Bueno Castellano Christina , Wilkins Victoria M. , Kanellopoulos Dora 
Published: November 2023

Abstract
This chapter introduces a cognitive behavioral model of COVID-19. It starts by providing an overview of COVID-19 and its persistent effects, such as thoughts, emotions, and behaviors that can perpetuate and worsen anxiety, depression, and emotional distress. This emotional distress can contribute to worsening adjustment and medical/rehabilitation results. In addition to thoughts, emotions, and behavioral responses, systemic and environmental stressors can influence mood and anxiety in the context of persistent COVID-19 symptoms. The chapter emphasizes the importance of home practice for the success of the treatment. Worksheets provide information about the cognitive behavioral model and allow the client to track thoughts, emotions, and responses to COVID-19 symptoms.
Module 4: Behavioral Activation
Authors: Jaywant Abhishek , Oberlin Lauren E. , Cherestal Stephanie , Bueno Castellano Christina , Wilkins Victoria M. , Kanellopoulos Dora 
Published: November 2023

Abstract
This chapter focuses on behavioral activation, a strategy that can be used to address depression in clients who have persistent symptoms of COVID-19. This strategy involves re-engaging in activities that the client previously enjoyed and starting new enjoyable or rewarding activities. The sense of achievement that the client experiences from participating in meaningful activities will enhance their outlook and improve their engagement in life, despite the limitations imposed by persistent COVID-19 symptoms. Putting these activities on a schedule increases the likelihood that the client will pursue them. Worksheets in this chapter focus on adapting, scheduling, and generating new activities for at-home practice.
Module 5: Mindfulness
Authors: Jaywant Abhishek , Oberlin Lauren E. , Cherestal Stephanie , Bueno Castellano Christina , Wilkins Victoria M. , Kanellopoulos Dora 
Published: November 2023

Abstract
This chapter introduces mindfulness as a technique for assisting clients with persistent COVID-19 symptoms to manage their emotional distress, anxiety, and depression. Mindfulness is defined as paying attention in a particular way: on purpose, in the present moment, and non-judgmentally. It is not necessarily about relaxation or clearing the mind but rather a process of bringing conscious, deliberate attention and awareness to moment-to-moment experiences. Clients can practice mindfulness by engaging in culturally relevant activities or by using mobile apps outside of the therapy session. Mindfulness techniques have been incorporated into evidence-based psychotherapies for psychiatric conditions and programs for managing chronic illness. The importance of at-home practice of mindfulness techniques is emphasized.
Module 6: Relaxation Skills
Authors: Jaywant Abhishek , Oberlin Lauren E. , Cherestal Stephanie , Bueno Castellano Christina , Wilkins Victoria M. , Kanellopoulos Dora 
Published: November 2023

Abstract
This chapter discusses how relaxation skills can help deal with stress associated with persistent COVID-19 symptoms. It explains the fight-or-flight response, also known as the acute stress response, which is a physiological or bodily response to a trigger (an event, situation, or worry) that is seen as stressful or frightening. Relaxation strategies are designed to decrease physical symptoms and alleviate acute stress. However, while relaxation is an effective approach for managing severe, acute distress, relaxation techniques should not be used to try to avoid all unwanted emotions and physical sensations. The chapter details several relaxation strategies, such as diaphragmatic breathing.
New evidence of multiple channels for the origin of gamma-ray bursts with extended emission
Authors: Li Q M , Sun Q B , Zhang Z B , Zhang K J , Long G 
Published: November 2023

ABSTRACT
Gamma-ray bursts (GRBs) are the most intense explosions in the Universe. GRBs with extended emission (GRBs EE) constitute a small subclass of GRBs. GRBs EE are divided into EE-I GRBs and EE-II GRBs, according to the Amati empirical relationship rather than duration. We test here if these two types of GRB have different origins based on their luminosity function (and formation rate). Therefore, we use Lynden-Bell’s c− method to investigate the luminosity function and formation rate of GRBs with EE without any assumption. We calculate the formation rate of two types of GRBs. For EE-I GRBs, the fitting function can be written as ρ(z) ∝ (1 + z)−0.34 ± 0.04 for z &lt; 2.39 and ρ(z) ∝ (1 + z)−2.34 ± 0.24 for z &gt; 2.39. The formation rate of EE-II can describe as ρ(z) ∝ (1 + z)−1.05 ± 1.10 for z &lt; 0.43 and ρ(z) ∝ (1 + z)−8.44 ± 1.10 for z &gt; 0.43. The local formation rate is $\rho (0) = 0.03\, {\rm Gpc}^{-3} \, {\rm yr}^{-1}$ for some EE-I GRBs and $\rho (0) = 0.32 \, {\rm Gpc}^{-3} \, {\rm yr}^{-1}$ for EE-II GRBs. Based on these results, we provide new evidence that the origins of EE-I GRBs are different from EE-II GRBs from the perspective of event rate. The EE-I GRB could be produced from the death of the massive star, but EE-II GRB may come from other processes that are unrelated to the star formation rate. Our findings indicate that the GRBs with EE could have multiple production channels.
Radial compositional profile of Saturn's E ring indicates substantial space weathering effects
Authors: Nölle Lenz , Postberg Frank , Schmidt Jürgen , Klenner Fabian , Khawaja Nozair , Hillier Jon , Kempf Sascha , Hsu Sean , Srama Ralf 
Published: November 2023

Abstract
Saturn's large and diffuse E ring is populated by microscopic water ice dust particles, which originate from the Enceladus plume. Cassini’s Cosmic Dust Analyser sampled these ice grains, revealing three compositional particle types with different concentrations of salts and organics. Here, we present the analysis of CDA mass spectra from several orbital periods of Cassini, covering the region from interior to Enceladus’ orbit to outside the orbit of Rhea, to map the distribution of the different particle types throughout the radial extent of the E ring. This will provide a better understanding of the potential impact of space weathering effects on to these particles, as the ice grains experience an increasing exposure age during their radially outward migration. In this context, we report the discovery of a new ice particle type (Type 5), which produces spectra indicative of very high salt concentrations, and which we suggest to evolve from less-salty Enceladean ice grains by space weathering. The radial compositional profile, now encompassing four particle types, reveals distinct radial variations in the E ring. At the orbital distance of Enceladus our results are in good agreement with earlier compositional analyses of E ring ice grains in the moon's vicinity. With increasing radial distance to Saturn however, our analysis suggests a growing degree of space weathering and considerable changes to the spatial distribution of the particle types. We also find that the proportion of Type 5 grains – peaking near Rhea's orbit – probably reflects particle charging processes in the E ring.
A systematic study of the high-frequency bump in the black-hole low-mass X-ray binary GX 339 − 4
Authors: Zhang Yuexin , Méndez Mariano , Motta Sara E , Zdziarski Andrzej A , Marcel Grégoire , García Federico , Altamirano Diego , Belloni (deceased) Tomaso M , Zhang Liang , Timmermans Thimo , Zhang Guobao 
Published: November 2023

ABSTRACT
The high-frequency bump, characterized by a frequency exceeding ∼30 Hz, represents a seldom-explored time-variability feature in the power density spectrum (PDS) of black-hole X-ray binaries. In the 2002, 2004, 2007, and 2010 outbursts of GX 339 − 4, the bump has been occasionally observed in conjunction with type-C quasi-periodic oscillations (QPOs). We systematically study the properties of the bump during these four outbursts observed by Rossi X-ray Timing Explorer (RXTE) in the 2–60 keV bands and detect the bump in 39 observations. While the frequencies of the type-C QPOs are in the range of ∼0.1–9 Hz, the root-mean-square (rms) amplitude of the bump shows an evolution in the hardness ratio versus the type-C QPO frequency plot. By comparing the rms amplitude of the bump with the corona temperature and simultaneous radio jet flux of the source, as previously studied in GRS 1915 + 105, we establish that in the hard state of GX 339 − 4, the bump is always strong, with the measurements of the rms amplitude in the range of 4–10 per cent. At the same time, the corona temperature is high and the radio flux is low. These findings indicate that, using the bump as a proxy, the majority of the accretion energy is directed towards the hot corona rather than being channeled into the radio jet. We discuss this phenomenon in terms of an inefficient energy transfer mechanism between the corona and jet in GX 339 − 4.
MBH binary intruders: triple systems from cosmological simulations
Authors: Sayeb Mohammad , Blecha Laura , Kelley Luke Zoltan 
Published: November 2023

ABSTRACT
Massive black hole (MBH) binaries can form following a galaxy merger, but this may not always lead to a MBH binary merger within a Hubble time. The merger time-scale depends on how efficiently the MBHs lose orbital energy to the gas and stellar background, and to gravitational waves (GWs). In systems where these mechanisms are inefficient, the binary inspiral time can be long enough for a subsequent galaxy merger to bring a third MBH into the system. In this work, we identify and characterize the population of triple MBH systems in the Illustris cosmological hydrodynamic simulation. We find a substantial occurrence rate of triple MBH systems: in our fiducial model, 22 per cent of all binary systems form triples, and $\gt 70{{\ \rm per\ cent}}$ of these involve binaries that would not otherwise merge by z = 0. Furthermore, a significant subset of triples (6 per cent of all binaries, or more than a quarter of all triples) form a triple system at parsec scales, where the three BHs are most likely to undergo a strong three-body interaction. Crucially, we find that the rate of triple occurrence has only a weak dependence on key parameters of the binary inspiral model (binary eccentricity and stellar loss-cone refilling rate). We also do not observe strong trends in the host galaxy properties for binary versus triple MBH populations. Our results demonstrate the potential for triple systems to increase MBH merger rates, thereby enhancing the low-frequency GW signals detectable with pulsar timing arrays and with LISA.
The Tully–Fisher relation from SDSS-MaNGA: physical causes of scatter and variation at different radii
Authors: Ristea A , Cortese L , Fraser-McKelvie A , Catinella B , van de Sande J , Croom S M , Swinbank A M 
Published: November 2023

ABSTRACT
The stellar mass Tully–Fisher relation (STFR) and its scatter encode valuable information about the processes shaping galaxy evolution across cosmic time. However, we are still missing a proper quantification of the STFR slope and scatter dependence on the baryonic tracer used to quantify rotational velocity, on the velocity measurement radius and on galaxy integrated properties. We present a catalogue of stellar and ionized gas (traced by H$\rm {\alpha }$ emission) kinematic measurements for a sample of galaxies drawn from the MaNGA Galaxy Survey, providing an ideal tool for galaxy formation model calibration and for comparison with high-redshift studies. We compute the STFRs for stellar and gas rotation at 1, 1.3 and 2 effective radii (Re). The relations for both baryonic components become shallower at 2Re compared to 1Re and 1.3Re. We report a steeper STFR for the stars in the inner parts (≤1.3Re) compared to the gas. At 2Re, the relations for the two components are consistent. When accounting for covariances with integrated v/σ, scatter in the stellar and gas STFRs shows no strong correlation with: optical morphology, star formation rate surface density, tidal interaction strength or gas accretion signatures. Our results suggest that the STFR scatter is driven by an increase in stellar/gas dispersional support, from either external (mergers) or internal (feedback) processes. No correlation between STFR scatter and environment is found. Nearby Universe galaxies have their stars and gas in statistically different states of dynamical equilibrium in the inner parts (≤1.3Re), while at 2Re the two components are dynamically coupled.
A generalized semi-analytic model for magnetar-driven supernovae
Authors: Omand Conor M B , Sarin Nikhil 
Published: November 2023

ABSTRACT
Several types of energetic supernovae, such as superluminous supernovae (SLSNe) and broad-line Ic supernovae (Ic-BL SNe), could be powered by the spin-down of a rapidly rotating magnetar. Currently, most models used to infer the parameters for potential magnetar-driven supernovae make several unsuitable assumptions that likely bias the estimated parameters. In this work, we present a new model for magnetar-driven supernovae that relaxes several of these assumptions and an inference workflow that enables accurate estimation of parameters from light curves of magnetar-driven supernovae. In particular, in this model, we include the dynamical evolution of the ejecta, coupling it to the energy injected by the magnetar itself while also allowing for non-dipole spin down. We show that the model can reproduce SLSN and Ic-BL SN light curves consistent with the parameter space from computationally expensive numerical simulations. We also show the results of parameter inference on four well-known example supernovae, demonstrating the model’s effectiveness at capturing the considerable diversity in magnetar-driven supernova light curves. The model fits each light curve well and recovers parameters broadly consistent with previous works. This model will allow us to explore the full diversity of magnetar-driven supernovae under one theoretical framework, more accurately characterize these supernovae from only photometric data, and make more accurate predictions of future multiwavelength emission to test the magnetar-driven scenario better.
A two-component clumpy model for the shell evolution of classical novae: the case of V5668 Sgr
Authors: Abraham Zulema , Takeda Larissa , Beaklini Pedro P B , Diaz Marcos , Page Kim L , Chomiuk Laura , Linford Justin D 
Published: November 2023

ABSTRACT
The shell of the classical nova V5668 Sgr was resolved by ALMA at the frequency of 230 GHz 927 d after eruption, showing that most of the continuum bremsstrahlung emission originates in clumps with diameter smaller than 1015 cm. Using Very Large Array radio observations, obtained between days 2 and 1744 after eruption, at frequencies between 1 and 35 GHz, we modelled the nova spectra, assuming first that the shell is formed by a fixed number of identical clumps, and afterwards with the clumps having a power-law distribution of sizes, and were able to obtain the clump’s physical parameters (radius, density, and temperature). We found that the density of the clumps decreases linearly with the increase of the shell’s volume, which is compatible with the existence of a second media, hotter and thinner, in pressure equilibrium with the clumps. We show that this thinner media could be responsible for the emission of the hard X-rays observed at the early times of the nova eruption, and that the clump’s temperature evolution follows that of the super-soft X-ray luminosity. We propose that the clumps were formed in the radiative shock produced by the collision of the fast wind of the white dwarf after eruption, with the slower velocity of the thermonuclear ejecta. From the total mass of the clumps, the observed expansion velocity and thermonuclear explosion models, we obtained an approximate value of 1.25 M⊙ for the mass of the white dwarf, a central temperature of 107 K and an accretion rate from the secondary star of 10−9–10−8 M⊙ yr−1.
X-ray polarization properties of thermal-radiative disc winds in binary systems
Authors: Tomaru Ryota , Done Chris , Odaka Hirokazu 
Published: November 2023

ABSTRACT
New X-ray polarization results are challenging our understanding of the accretion flow geometry in black hole binary systems. Even spectra dominated by a standard disc can give unexpected results, such as the high-inclination black hole binary 4U 1630−472, where the observed X-ray polarization is much higher than predicted. This system also shows a strong, highly ionized wind, consistent with thermal-radiative driving from the outer disc, leading to speculation that scattering in the wind is responsible for the unexpectedly high polarization degree from a standard optically thick disc. Here, we show that this is not the case. The optically thin(ish) wind polarizes the scattered light in a direction orthogonal to that predicted from a standard optically thick disc, reducing about 2 per cent rather than enhancing the predicted polarization of the total emission. This value is consistent with the polarization difference between the disc-dominated soft state, where absorption lines by the wind are clearly seen, and the steep power-law state, where no absorption lines are seen. If this difference is genuinely due to the presence or absence of wind, the total polarization direction must be orthogonal to the disc plane rather than parallel as expected from optically thick material.
The accretion history of the Milky Way: III. Hydrodynamical simulations of Galactic dwarf galaxies at first infall
Authors: Wang Jianling , Hammer Francois , Yang Yanbin , Pawlowski Marcel S , Mamon Gary A , Wang Haifeng 
Published: November 2023

ABSTRACT
Most Milky Way dwarf galaxies are much less bound to their host than are relics of Gaia–Sausage–Enceladus and Sgr. These dwarfs are expected to have fallen into the Galactic halo less than 3 Gyr ago, and will therefore have undergone no more than one full orbit. Here, we have performed hydrodynamical simulations of this process, assuming that their progenitors are gas-rich, rotation-supported dwarfs. We follow their transformation through interactions with the hot corona and gravitational field of the galaxy. Our dedicated simulations reproduce the structural properties of three dwarf galaxies: Sculptor, Antlia II, and with somewhat a lower accuracy, Crater II. This includes reproducing their large velocity dispersions, which are caused by ram-pressure stripping and Galactic tidal shocks. Differences between dwarfs can be interpreted as due to different orbital paths, as well as to different initial conditions for their progenitor gas and stellar contents. However, we failed to suppress in a single orbit the rotational support of our Sculptor analogue if it is fully dark matter dominated. In addition, we have found that classical dwarf galaxies like Sculptor may have stellar cores sufficiently dense to survive the pericentre passage through adiabatic contraction. On the contrary, our Antlia II and Crater II analogues are tidally stripped, explaining their large sizes, extremely low surface brightnesses, and velocity dispersion. This modelling explains differences between dwarf galaxies by reproducing them as being at different stages of out-of-equilibrium stellar systems.
Multistream radial structure of cold dark matter haloes from particle trajectories: deep inside splashback radius
Authors: Enomoto Yohsuke , Nishimichi Takahiro , Taruya Atsushi 
Published: November 2023

ABSTRACT
By tracking trajectories of dark matter (DM) particles accreting on to haloes in cosmological N-body simulations, we investigate the radial phase-space distribution of cold dark matter (CDM) haloes, paying attention to their inner regions deep inside the halo boundary called the splashback radius, where the particles undergo multistream flows. Improving the analysis by Sugiura et al., we classify DM particles by the number of apocentre passages, p, and count it up to p = 40 for each halo over a wide mass range. Quantifying the radial density profile for particles having the same value of p, we find that it generally exhibits a double power-law feature, whose indices of inner and outer slopes are well described by −1 and −8, respectively. Its characteristic scale and density are given as a simple fitting function of p, with a weak halo mass dependence. Interestingly, summing up these double power-law profiles beyond p = 40 reproduces well the total density profile of simulated haloes. The double power-law nature is persistent and generic not only in mass-selected haloes but also in haloes selected in different criteria. Our results are compared with self-similar solutions that describe the stationary and spherical accretion of DM. We find that even when introducing a non-zero angular momentum, none of them explain the radial multistream structure. The analysis with particle trajectories tracing back to higher redshifts suggests that the double power-law nature has been established during an early accretion phase and remains stable.