This may imply that the shock properties responsible for the γ-ray emission in V549 Vel are different from those of the more luminous events. In this work, to complement our previous study on a similar topic, we perform nonlinear time series analysis of the decade-long Fermi/LAT observations of 20 γ-ray bright blazars. We use a combination of full-disk data from the Solar Dynamics Observatory and high-resolution data from the Dunn Solar Telescope (DST) to study the formation, structure, and evolution of an atypical light bridge (LB) in a regular sunspot. Sang-Yoon Lee, Chul Chung, and Suk-Jin Yoon. Xinting Yu (余馨婷), Sarah M. Hörst, Chao He, Patricia McGuiggan, Kai Kristiansen, and Xi Zhang. We used the 12CO and 13CO J = 1–0 data from the Milky Way Image Scroll Painting CO line survey to search for molecular gas associated with G57.2+0.8, in order to constrain the physical parameters (e.g., the distance) of the SNR and its magnetar. Interestingly, The CS is dynamically linked to a massive globular cluster, NGC 5824. Both signals are affected by contamination at small angular scales due to extragalactic radio sources (the former) and dusty star-forming galaxies (the latter). Dusty plasma analysis shows that an ice grain is charged to a negative potential that has magnitude nearly equal to that of the electron temperature. This suppresses buildup of material at the center, causing the RC to rise more slowly and reducing the central LOSVD. Improvements in astrometric and spectroscopic measurements have made it possible to detect BHs also in noninteracting BH binaries (nBHBs) through a precise analysis of the companion's motion. Combined with observations of the atomic carbon (C i) and carbon monoxide (CO J = 4–3) in the same system, we reveal the conditions in this intensely star-forming system. Generally speaking, there are two classes of outflows—subsonic and supersonic (with respect to a suitably defined sound speed). On larger scales, we identify, for the first time, a steep density spectrum in the diffuse WIM extending up to several kiloparsecs. Lorena Carmo, Diego F. González-Casanova, Diego Falceta-Gonçalves, Alex Lazarian, Francisco Jablonski, Jian-Fu Zhang, Ivan Ferreira, Manuel Castro, and Bo Yang. Using the case study of biosignature yields calculated for θ Cygni and 55 Cancri, we find that robust mission design and target selection for HabEx and LUVOIR depend on choosing a specific model of biosignature appearance with time, the terrestrial planet occurrence rate as a function of orbital separation, precise knowledge of stellar properties, and accurate stellar evolutionary histories. The Taffy Galaxy system (UGC 1294/5) is a prototypical example of a splash bridge system. The height–time evolution and velocity profiles of the simulation inflows and in/out pairs are compared to their corresponding observations and a detailed analysis of the underlying magnetic field structure associated with the synthetic white-light and mass density evolution is presented. We explore the ability in magnetic field tracing of gradients of higher-order velocity centroids and compare their performance with that of traditional velocity centroid gradients (VCGs) and with intensity gradients (IGs). The upper limit on sin2(2θ) is (though systematic uncertainty may increase this by a factor of ~2), corresponding to an upper limit on 3.5 keV line flux of photons s−1 cm−2. Lensing reconstructions reveal that 500 pc scale clumpy structures in the outflows are common. To measure the magnetization level, Lazarian et al. John E. Vaillancourt, B-G Andersson, Dan P. Clemens, Vilppu Piirola, Thiem Hoang, Eric E. Becklin, and Miranda Caputo. These methods are promising, but performing the necessary calculations can be computationally intensive and algebraically tedious. When we force only kinetically, negative η yx are obtained with exponential growth in both the radial and azimuthal mean magnetic field components. Here we show that stochastic interactions between the ionizing radiation from the BH and nonuniform accretion flow can lead to the formation of a rotating gas disk around the BH. Merger Characteristics, Study Turbulence and Probe Magnetic Fields Using the Gradient Technique: Application to H, Synchrotron Intensity and Polarization Gradients: Tools to Obtain the Magnetization Level in a Turbulent Medium, JWST Transit Spectra. However, current and upcoming wide-field time-domain surveys have increased the transient discovery rate far beyond our capacity to obtain even a single spectrum of each new event. Furthermore, the presence of electric charges induces the generation of electric currents and high magnetic fields. The high temperatures require energy to be carried from the solar interior to the corona by non-thermal processes, because the second law of thermodynamics prevents heat from flowing directly from the solar photosphere (surface), which is at about 5800K, to the much hotter corona at about 1 to 3 MK (parts of the corona can even reach 10MK). We hypothesize an unseen circumbinary companion responsible for the cavity in scattered light and creating a vortex at the cavity edge that manifests in dust trapping. The method employs two physical properties of the expanding solar wind plasma, the wave-particle thermodynamic equilibrium, and the transport of entropic rate. If you have a user account, you will need to reset your Jesse Bluem, Philip Kaaret, William Fuelberth, Anna Zajczyk, Daniel M. LaRocca, R. Ringuette, Keith M. Jahoda, and K. D. Kuntz. Fast radio bursts (FRBs) are a new kind of extragalactic radio transients. The outflows appear to be primarily photoionized by the AGN rather than shocks or young, massive stars. The structure was observed in a broad range of temperatures and it moved along the rope with the velocity of about 240 km s−1. is the Debye length of the plasma with particle density Expatica is the international community’s online home away from home. Our optical (BVRI) polarimetric campaign shows variable linear polarization (LP) throughout the outburst. This site uses cookies. We compare the performance of the standard diffusive inpainting with that of two novel methodologies relying on DCNNs, namely Generative Adversarial Networks and Deep-Prior. The mass, momentum, and energy of individual outflows in Perseus predicted by model MF is comparable to the previous estimations. These stars appear to be coeval and relatively massive. We study ram pressure stripping in simulated Milky Way-like halos at from the Figuring Out Gas & Galaxies in Enzo (FOGGIE) project. Joshua J. Hibbard, Keith Tauscher, David Rapetti, and Jack O. Burns. Moreover, no more than <57% (<89%) of putative kilonovae could be brighter than −16.6 mag assuming flat evolution (fading by 1 mag day−1) at the 90% confidence level. In the hard X-ray range, bursts are recorded with RHESSI channels up to 25 keV. The scatter in the L [C ii]–SFR relation is mostly driven by galaxy properties, such that at a given SFR galaxies with higher molecular mass and metallicity have higher L [C ii]. Duo Xu, Stella S. R. Offner, Robert Gutermuth, and Colin Van Oort. The LB results from the emergence of magnetic flux with one footpoint rooted in a pore outside the parent sunspot that appears about 17 hr before the LB. When adopting the Gaia distance, the spectral energy distribution of the progenitor is close to that of a G-type star. But this is exactly what happens in a tidal disruption event," … These mechanisms include the focusing of water molecule trajectories, the migration of water molecules in a quasi-liquid layer on the grain surface toward regions where the electric field is strongest, the enhancement of this migration by the bombardment of energetic protons that gain energy upon falling into the ice grain negative potential, and mutual repulsion by electric charges having the same sign. A total of 103 flare stars are detected, of which 72 have the Large Sky Area Multi-Object fiber Spectroscopic Telescope spectral types, resulting in 51 A-type stars, including 17 new and 34 known. Energy cannot be transferred from the cooler photosphere to the corona by conventional heat transfer as this would violate the second law of thermodynamics. The magnetic energy in MADs is higher than the thermal energy of the accreting plasma, where the magnetic reconnection or turbulence may efficiently accelerate nonthermal protons. We use a model of the infall pattern of the local Hubble flow modified by the Virgo mass, which is given as a function of the cosmological constants (H 0, ΩΛ), the radius of the zero-velocity surface R 0, and the intrinsic velocity dispersion, σ v . All data are modeled using both background-subtracted and background-modeled approaches to account for the particle instrument background, demonstrating the statistical limitations of the currently available ~1 Ms of particle background data. Modeling of the dust continuum and spectral energy distribution yields a disk mass of 0.035 M ⊙ (inferred dust+gas) and a dust disk radius of 62 au; thus, the dust disk may have a smaller radius than the gas disk, similar to Class II disks. The result, with possible implication of strong disk-jet connection in blazars, could prove to be significantly useful in constructing models that can explain the rich and complex multiwavelength observational features in active galactic nuclei. Furthermore, by estimating the rate of transients with light curves similar to that of AT 2020blt in ZTF high-cadence data, we agree with previous results that there is no evidence for an afterglow-like phenomenon that is significantly more common than classical GRBs, such as dirty fireballs. , Is NGC 5824 the Core of the Progenitor of the Cetus Stream? We derive the photospheric and chromospheric structure of the LB in the DST data from spectral line parameters and inversions of He i at 1083 nm, Si i at 1082.7 nm, Ca ii IR at 854 nm, and H α at 656 nm and speckle-reconstructed imaging at 700 and 430 nm. e Splash bridges are created from the direct collision of two gas-rich disk galaxies. We first simulate it in isolation for 6 Gyr, starting from an initial good match to the rotation curve (RC). The gas mass evolution of a minihalo can be characterized by a scaling parameter that is given by a combination of the halo mass, background radiation intensity, and redshift. The idea that nanoflares might heat the corona was proposed by Eugene Parker in the 1980s but is still controversial. Significant emissions of all three lines are detected along the so-called nuclear spiral across the central kiloparsec of M31. They not only propagated much faster than the local Alfvén speed of about 260 km s−1, but also were simultaneously accompanied by a type II radio burst, i.e., a typical feature of a shock wave. In our setup, a negative sign of its component η yx is necessary for coherent dynamo action by the SC effect. It is hypothesized that the reconnection and unravelling of braids can act as primary sources of heating of the active solar corona to temperatures of up to 4 million kelvin. The smooth component of the bursts dominated at 17 GHz and was emitted by bremsstrahlung. Why is the Sun's corona so much hotter than the Sun's surface? We gathered multiepoch high-resolution spectra of each target, and we measured equivalent widths of the activity indicators helium I D3, Hα, and the calcium infrared triplet line at 8542.09 Å. We conclude by discussing the status and future of fast-transient searches in wide-field high-cadence optical surveys. The radial velocity method is one of the most successful techniques for the discovery and characterization of exoplanets. The progenitor was also observed by the 2MASS and WISE surveys. Here we present the first FIR spectroscopic mapping of the circumnuclear region of M31 in [C ii] 158 μm, [O i] 63 μm, and [O iii] 88 μm lines with the Herschel Space Observatory, covering an ~500 × 500 pc (2' × 2') field. The model suggests no or little radial variation in GC age even out to ~20 R eff. Here we explore in more detail the possible systematics of such a merger and a larger range of accreted masses. The composition is similar to that in the Sun's interior, mainly hydrogen, but with much greater ionization than that found in the photosphere. We find unambiguous evidence for outflows in 8/11 galaxies (73%), more than tripling the number known at z > 4. Magnetic reconnection is hypothesized to be the mechanism behind solar flares, the largest explosions in the Solar System. We aim to better understand the conditions for star formation in splash bridges by employing a Jeans criterion to determine where gravitational instabilities occur in the shocked and cooling gas of gas-rich disk collisions. We derive analytical models of the mass-weighted hydrogen ionization fraction from the local ionization balance equations as a more accurate alternative to the widely adopted model based on the volume filling factor. But because this is a UV-selected sample, we are missing [C II]-bright but UV-faint sources, making our constraints strict lower limits. For the two relatively bright A-type flare stars, KIC 5360548 and KIC 9468475, three high-resolution spectra are observed on different nights for each of them, and radial velocities are calculated and compared with that of the previous research. Coronal waves exist ubiquitously in the solar atmosphere. This combines to give <1% false probability of the OH maser, suggesting a real maser detection. A living nightmare surrounds her, the terrible breeze slamming … Current sheets are dominant in the highly disturbed period, wave packets are the most common in the quiet interval; while, in the weakly disturbed period, a mixture of vortices and wave packets is observed. Amazon Music Stream millions of songs: Amazon Advertising Find, attract, and Merger Characteristics, , Study Turbulence and Probe Magnetic Fields Using the Gradient Technique: Application to H i-to-H2 Transition Regions, , Synchrotron Intensity and Polarization Gradients: Tools to Obtain the Magnetization Level in a Turbulent Medium, , JWST Transit Spectra. In addition, we estimate the dynamical timescales, so-called trapping timescales, in the order of a few weeks. A suggestive scenario is that NGC 5824 was the nuclear star cluster of the dwarf progenitor of the CS. The term-dependent one-electron orbitals in the multiconfiguration Hartree–Fock approach with adjustable configuration expansions and semi-empirical fine-tuning for energy corrections have been used in achieving highly accurate target description. Using the spectra and their covariance estimated from N-body simulations, we find that the multitracer approach is effective in reducing the cosmic variance noise. The density distribution of the intergalactic medium is an uncertain but highly important issue in the study of cosmic reionization. The other three radii are taken from the simulation and use the disk rotation, infall motion, and density contrast around the protostar to identify the disk. However, no GRB was detected in the 0.74 days between the last ZTF nondetection (r > 21.36 mag) and the first ZTF detection (r = 19.60 mag), with an upper limit on the isotropic-equivalent gamma-ray energy release of E γ,iso < 7 × 1052 erg. In recent years, a few dozen such flares have been discovered, but they are not well understood. Each of these quantities varies significantly with stellar mass and stellar age, but we are able to reduce all of our simulations to a single relationship that depends only on stellar structure, characterized by a single parameter , and impact parameter β. The system maintains a quasi-self-similar evolution in time, which serves as a proxy for understanding the underlying physical mechanisms driving it. of the field line, becomes. Thus they appear to have neither chromospheres nor coronae. What astronomers may be witnessing is a "tidal disruption" event, which happens when the huge gravitational force of a black hole rips a nearby star into streams of gas. Hence, they provide a unique opportunity to study the properties of these ‘hidden’ black holes … The slope sign change is related to the knee of the FUV LF. In addition to redshift dependence, we also see the dependence of the ionized hydrogen clumping factor on ionization fraction, and we incorporate this into our fits. A charged particle moving in the direction perpendicular to the magnetic field line is subject to the Lorentz force which is normal to the plane individuated by the velocity and the magnetic field. A three-fluid model without cosmic-ray diffusion can be studied in the same way as the classic stellar wind problem, and is taken as a reference model. We then add a constant external acceleration field of 8.4 × 10−12 m s−2 at 30° to the disk as a first-order estimate for the gravity exerted by M31. In this scenario, the frequency drifting is mainly caused by the geometric structure of a pulsar magnetosphere, and the drifting rate–frequency index is found to be 25/17. An instant interpretation is that there exist two distinct GC subsystems having different radial distributions. The pore has a polarity opposite to that of the sunspot and recedes from it at a speed of about 0.4 km s−1. The above trends are consistent with the scenario where the dynamical environment is relatively colder for more massive structures because their own gravity is more likely to dominate the local potentials. Combining local and global aspects, we conclude that the formation of G33.92+0.11 is predominantly driven by gravity, dragging and aligning the major filaments and magnetic field on the way to the inner dense center. Gaia detected a candidate progenitor of V549 Vel and found a parallax measurement of  = 1.91 ± 0.39 mas, equivalent to a mode distance of d ≈ 560 pc (90% credible interval of 380–1050 pc). Here we report James Clerk Maxwell telescope POL-2 850 μm polarization and IRAM 30 m C18O (2–1) line observations toward the massive HFS G33.92+0.11. {\displaystyle m_{e}} Further simulations with a time-varying external field, modeling the full orbit of M33, will be needed to confirm its resemblance to observations. Observations, however, increasingly challenge this and other basic expectations. We also propose an effective equation of state that models the multiphase ISM formed by the WNM converging flow as a one-phase ISM in the form of P ∝ ργ eff , where γ eff varies from 0.9 (for a large pre-shock Δρ 0) to 0.7 (for a small pre-shock Δρ 0). The Sérsic values also increase for the massive star-forming galaxies toward late cosmic time. contents in brief. However, following observational research in the 1980s, it was found that spicule plasma did not reach coronal temperatures, and so the theory was discounted. These observations suggest that the CSB is a cohesive object with a singular origin. B With the rich multiwavelength data in the HSC deep fields, we then confirm that the selected galaxies are in the targeted redshift range of 1 < z < 1.5, lie in the passive region of the UVJ diagram, and have high stellar masses at log(M */M ⊙) > 10.5, with a median of log(M */M ⊙) = 11.0. Stellar orbits in the centre of a galaxy are not static, and sometimes stars walk into trouble. It is thought that the fast-mode shock triggered EMR in the null point region and caused the subsequent eruptions. One major goal of gravitational-wave astronomy is to detect gravitational waves from coalescing massive black hole binaries. We show that when dusty plasma effects and the dipole moment of water molecules are together taken into account, ice grains in interstellar space should be prolate ellipsoids and not spheres. This vindicates the model and simplifying assumptions used. Is NGC 5824 the Core of the Progenitor of the Cetus Stream? These wide array of transitions give rise to many main Ti II infrared, optical, and ultraviolet lines from a variety of astrophysical objects. Assuming that Si ii, Si iii, and Si iv comprise nearly 100% of the total silicon, we find 3% (~8 × 103 M ⊙), 2% (~7 × 103 M ⊙), and 32%–42% [~(1.0–1.3) × 105 M ⊙] of the silicon mass in the stars, interstellar medium, and within 0.6R 200 of the CGM of IC 1613. Our derived dust-obscured fractions agree with previous determinations at 0 ≤ z ≤ 2.5.
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