Astrophysics and Space Science最新文献

This paper traces the 37 years of my career dedicated to the development of integral field spectroscopy (IFS), highlighting significant milestones and advancements. This extensive journey encompasses three generations of IFS: the initial prototype TIGER at CFHT, the first generation including OASIS at CFHT and SAURON at WHT, the second generation with MUSE at VLT, and the potential third generation represented by the Wide-field Spectroscopic Telescope (WST) project. Throughout, I discuss the lessons learned at each stage and provide my perspective on the future of IFS.

Solar images are critically important for studying solar activities and features. Today, many observatories rely on CMOS sensors to acquire these images. However, these sensors often introduce column fixed-pattern noise (CFPN), seriously affecting image quality. Therefore, we proposed a two-way filtering algorithm to remove CFPN. Firstly, in the horizontal direction, we used the one-dimensional global weighted least squares filter and the efficient bilateral filter to obtain a coarse denoised image. Then, we utilized the weighted guided filter in the vertical direction to estimate the CFPN components, thereby obtaining a clean solar image. We selected three different solar observation images to compare and evaluate our results to those obtained by three comparative methods. The images are observed by the Solar Upper Transition Region Imager aboard the SATech-01 satellite. Additionally, we further used two quantitative metrics, photo response non-uniformity and mean relative deviation, to quantify the denoised results. The results demonstrate that our proposed method removes the CFPN better and preserves the image features in a more balanced way.

A total solar eclipse occurred on April 8, 2024, across the United States, with obscuration rates ranging from 20–100% at different locations. We study the ionospheric Total Electron Content (TEC) response to the eclipse using data from 51 ground-based GPS stations. We find a significant depletion in TEC of up to 65%, with larger depletion rates occurring along the path of totality. We also observe a time delay between the maximum TEC depletion and the time of maximum obscuration, ranging from 8 to 80 minutes, with longer delays occurring at stations with lower obscuration rates. Both time delay and TEC depletion rates are found to vary with latitude, with slightly longer delays at lower latitudes and higher TEC depletion rates at mid-latitudes. The TEC depletion rate also increased with local time, showing a higher decrement after noon compared to before. The spatiotemporal variation in TEC closely followed the eclipse’s path, indicating a positive correlation with the movement of the moon’s shadow. Monitoring rate of TEC change during such rare events is crucial for enhancing our understanding of ionospheric dynamics, which can be very helpful to improve the accuracy of global communication and navigation systems.

The unified model of jetted active galactic nuclei (AGNs) based on intrinsic properties presumes that the blazar subtypes of BL Lacertae objects (BLs) and flat-spectrum radio quasars (FSRQs) are aligned equivalents of Fanaroff–Riley type I (FR I) and Fanaroff–Riley type II (FR II) radio galaxies (RGs) from where their parent sources are obtained. Using compiled radio, X-ray and (gamma )-ray data of 397 Fermi Large Area Telescope (Fermi-LAT) blazars and 153 non-Fermi detected RGs, we computed the (gamma )-ray core-dominance parameter (R_γ) and (gamma )-ray emission components (beamed and unbeamed) to study the consequences of relativistic beaming and orientation effects on (gamma )-ray properties of radio RGs, BLs and FSRQs. Data analysis shows that the distributions of R_X and R_γ, on average, are consistent with the prediction of the unified scheme in which FSRQs and BLs are strongly beamed and inclined at smaller angles than RGs. Through statistical tests with chance probability, (p < 0.05), we find that the distributions of R_X and R_γ for radio galaxies and the blazar subtypes are not significantly different. There is a regular positive trend ((r > +0.60)) in the variation of radio core-dominance parameter – X-ray luminosity ((R - L_{mathrm{x}})) data from radio galaxies to FSRQs through BLs, which suggests that radio galaxies could be relativistically less beamed population of jetted AGNs. The results are consistent with the unified model for radio galaxies and the conventional blazar subtypes.

Stellar halos of galaxies retain crucial clues to their mass assembly history. It is in these galactic components that the remains of cannibalised galactic building blocks are deposited. For the case of the Milky Way, the opportunity to analyse the stellar halo’s structure on a star-by-star basis in a multi-faceted approach provides a basis from which to infer its past and assembly history in unrivalled detail. Moreover, the insights that can be gained about the formation of the Galaxy not only help constrain the evolution of our Milky Way, but may also help place constraints on the formation of other disc galaxies in the Universe. This paper includes a summary of work undertaken during a PhD thesis aiming to make progress toward answering the most fundamental question in the field of Galactic archaeology: “How did the Milky Way form?” Through the effort to answer this question, we summarise new insights into aspects of the history of assembly and evolution of our Galaxy and measurements of the structure of various of its Galactic components.

We present the first pulsation analysis of four totally eclipsing Algol systems S Cnc, SS Cet, TW And, and VW Cyg using the latest data available from Kepler (K2), and TESS databases. Based on the characteristics observed they are classified to be oscillating eclipsing Algol binaries with primary components having (gamma ) Dor type pulsations. The photometric solutions were derived for five Algols including TT Hya using Wilson-Devinney code (v2015), and the absolute parameters of all Algols in study were computed. The period variation study was also conducted using the O-C diagram and the variation is correlated either to mass loss or mass transfer or presence of third body in these systems. All the available IUE high and low resolution spectra for S Cnc, TT Hya as well as VBT and LAMOST spectra for SS Cet were used to measure the equivalent widths of prominent lines, and their significance is presented. Based on the photometric, spectroscopic, period variation, and pulsation studies the evolutionary scenario of all the five Algols is discussed using (T_{mathrm{eff}}) - Luminosity, q-r and q-p diagrams.

In this research paper we investigated the halo coronal mass ejections and sunspot number during the period December 2019 to December 2023 for the rising phase of solar cycle 25. The SOHO/LASCO instrument observed 145 HCMEs during this period. We selected 145 halo CMEs and the associated flares, SSN and Dst. The HCME is found to be significantly faster and more energetic than the other CME. During solar maximum, HCME occur more frequently. Here we have considered all the frontside disk halos, frontside limb halos and the backside halos of the sun. These halos are classified according to their source location. Mostly the frontside disk halos are more geoeffective. For 70% (7/10) of the halo CMEs associated with X class flares have a speed greater than 1000 km/s. The daily sunspot number (SSN) and the yearly mean total sunspot number are taken into consideration for our study. The study of sunspot numbers is essential for planning space-related activities, particularly for low Earth orbiting spacecraft. Geoeffectiveness is the capacity of HCMEs to induce geomagnetic storms. The “Dst (Disturbance storm time) index” is one geomagnetic metric that is used to measure this. We categorized geoeffective halos into three groups: strongly geoeffective (Strong-GE, Dst < −100 nT), moderately geoeffective (Moderate-GE, −100 < Dst ≤ −50 nT), and weakly geoeffective (Weak-GE, Dst > −50 nT). Only 3.44% of halo CMEs were strongly geoeffective, and all of these were disk halos. The NW quadrant has the highest number of events throughout the research period of December 2019–December 2023. In this paper, we illustrate how the parameters of halo coronal mass ejections, sunspots and Dst can be used for space weather effects, evaluating geoeffectiveness, and auroras.

In this study, we analyzed photometric data in the o- and c-band of the asteroid (3200) Phaethon from the ATLAS network from 2015 to 2024. Apparent magnitudes and phase angles were used to construct phase curves. Annual data sets were analyzed if the phase angle range was at least 15 degrees. The phase coefficients for 2021 and 2022 were negative and positive, respectively. Negative coefficients are unusual for asteroids and likely result from variations in the observed hemisphere due to changes in the viewing angle relative to Phaethon’s rotation axis. In 2021, the northern hemisphere was observed, while in 2022 the southern hemisphere was observed. In December 2017, negative slopes G were derived from the VRI phase curves, corresponding to a sub-Earth latitude of 46 degrees N. Using the G value in the R-band, we have obtained the approximate parameters of the Hapke model for the northern hemisphere of Phaethon, suggesting that its surface consists of particles with similar porosity or size distribution, a rougher surface, and stronger backward scattering compared to typical low-albedo asteroids, and possibly also compared to the southern region. The northern hemisphere of Phaethon is likely redder than its southern hemisphere, which is supported by the absolute color c-o estimates in 2022 showing that the southern region is bluer than the solar twin YBP 1194, the main-belt comet 107P/Wilson-Harrington, and even than the C-type asteroid (10) Hygiea. In 2022, the relative phase coefficients indicate a phase bluing effect, where Phaethon becomes bluer as the phase angle decreases.

We have carried out a detailed study of the Gamma-Ray Burst (GRB) photospheric emission model predicting a quasi-blackbody spectrum slightly broader than a Planck function. This model was suggested within the relativistic fireball dynamics for interpreting a still not well understood thermal component in the GRB prompt emission, recently observed by the GBM (Gamma-ray Burst Monitor) on board the Fermi space telescope. We propose a Monte Carlo (M C) code for elucidating the observed spectrum, the outflow dynamics and its geometry for a basic and a structured plasma jets whose parameters are implemented. The code involves a simulation part describing the photon propagation assuming an unpolarized, non-dissipative relativistic outflow and a data analysis part for exploring main photospheric emission properties such as the energy, arrival time and observed flux of the simulated seed photons and the photospheric radius. Computing the latter two observables by numerical integration, we obtained values very concordant with the M C simulated results. Fitting Band functions to the photon spectra generated by this method, we derived best-fit values of the photon indices matching well those featuring the observed spectra for most typical GRBs, but corresponding to fit functions inconciliable with blackbody spectral shapes. Various derived results are reported, compared to previous ones and discussed. They show to be very sensitive to the structure of the Lorentz factor that plays a crucial role in determining the presence and strength of geometrical effects. The latter manifest themselves by large broadenings of the simulated spectra featured by multiple peak energies consistently with GRB observations. They are assumed, with multiple Compton scattering, to produce bumps pointed out at very low photon energies. The interpretation of GRB observations is further performed via a Band spectral analysis using the RMFIT software. Finally, developments of this work are put into perspective.

In a recent series of papers, Leibowitz revealed two pacemaker frequencies associated with flares observed near the Sgr A* location: one for X-ray flares and the other for IR (infrared) flares. He proposed an astrophysical model to account for these two frequencies, involving a unique body orbiting the Sgr A* black hole (supposed nonrotating) close to its last stable circular orbit. In the framework of this model, the Roche lobe contacts the star’s surface near the periastrons, which generates matter pullouts. The resulting X events are then separated by time intervals that are close to integer multiples of the radial orbital frequency, which explains the X pacemaker. One revisits this X sequence orbiting-body interpretation but in a full general relativistic framework, which is more appropriate than the pseudo-Newtonian Paczyński-Wiita potential approach used by Leibowitz. One concludes that no main sequence (or giant) star can survive the tidal effects, whereas no pullout matter is possible for white dwarfs (or neutron stars), on the orbits compatible with the X pacemaker frequency, even if large eccentricities are allowed. This confirms the result obtained by Leibowitz (on the impossibility of a main sequence or usual compact star, since the only solution he found involves an “unusual internal structure star”) but (1) in the framework of full relativistic calculations and (2) extending the result to the eccentric case.