arXiv subjects

D. Savchenko

Publications and source records attributed to D. Savchenko.

13 recordsLinked to original sources

arXiv2026

Seyfert galaxy targets for KM3NeT neutrino telescope

Neutrino signal from a population of Seyfert galaxies has been detected by IceCube neutrino telescope in the muon neutrino channel that has sensitivity mostly to the Northern Hemisphere sources. This detection can be verified by KM3NeT telescope that has sensitivity also in the Southern Hemisphere. We define a catalog of Seyfert galaxies that are expected to be detectable with KM3NeT, assuming that the neutrino luminosity scales with the intrinsic hard X-ray luminosity of the sources. We find that four sources: NGC 1068, NGC 4151, NGC 4945 and Circinus galaxy, are detectable by KM3NeT, if their spectra follow either NGC 1068 or NGC 4151 spectral template based on IceCube data. We discuss uncertainties of the neutrino flux estimate, considering the Compton-thick nature of three of the four detectable sources: NGC 1068, NGC 4945 and Circinus. The limited catalog of the four sources can be used in KM3NeT source search to reduce the trial factor of analysis aimed at independent verification of the neutrino signal from Seyfert galaxies.

astro-ph.HE↗

arXiv2025

Neutrino emission and corona heating induced by high-energy proton interactions in Seyfert galaxies

Recent detection of very-high-energy neutrino emission from Seyfert type active galactic nuclei (AGN) provides a new insight into the physics of the AGN central engines. We notice that if high-energy protons responsible for neutrino emission are accelerated close to the surface of the accretion disk, the neutrino flux may have no unambiguously identifiable electromagnetic counterpart. This is because the electromagnetic power released in interactions of high-energy protons would only contribute to the heating of the disk surface and corona above the disk, rather than escape from the source. Given that the heat deposited in the corona is released in the hard X-ray range we notice that there still might be an "indirect" electromagnetic counterpart of the neutrino signal: the hard X-ray flux variability may be strongly or weakly correlated with the neutrino flux variations, depending on the importance of the high-energy proton heating in the disk/corona heat balance. If heating by high-energy protons provides a sizable contribution to the overall corona heating rate, the overall flux of diffuse GeV neutrino background from Seyfert galaxies may be comparable to the X-ray background flux and the high-energy tail of this background can provide a sizable contribution to the astrophysical neutrino flux in the TeV band.

astro-ph.HE↗

arXiv2023

Neutrino signal from Cygnus region of the Milky Way

Interactions of cosmic ray protons and nuclei in their sources and in the interstellar medium produce "hadronic" gamma-ray emission. Gamma-rays can also be of "leptonic" origin, i.e. originating from high-energy electrons accelerated together with protons. It is difficult to distinguish between hadronic and leptonic emission mechanisms based on gamma-ray data alone. This can be done via detection of neutrinos, because only hadronic processes lead to neutrino production. We use publicly available ten-year IceCube neutrino telescope dataset to demonstrate the hadronic nature of high-energy emission from the direction of Cygnus region of the Milky Way. We find a 3-sigma excess of neutrino events from an extended Cygnus Cocoon, with the flux comparable to the flux of gamma-rays in the multi-TeV energy range seen by HAWC and LHAASO telescopes.

astro-ph.HE↗

arXiv2023

The study of x-ray spectrum of the Coma cluster

The X-ray spectrum of the Coma galaxy cluster was studied using the data from the XMM-Newton observatory. We combined 7 observations performed with the MOS camera of XMM-Newton in the 40'x 40' region centered at the Coma cluster. The analyzed observations were performed in 2000-2005 and have a total duration of 196 ksec. We focus on the analysis of the MOS camera spectra due to their lower affection by strong instrumental line-like background. The obtained spectrum was fitted with a model including contributions from the Solar system/Milky Way hot plasma and a power law X-ray background. The contribution of the instrumental background was modeled as a power law (not convolved with the effective area) and a number of Gaussian lines. The contribution from the Coma cluster was modeled with a single-temperature hot plasma emission. In addition, we searched for possible non-thermal radiation present in the vicinity of the center of the Coma cluster, originating e.g. from synchrotron emission of relativistic electrons on a turbulent magnetic field. We compared the results with previous works by other authors and spectra obtained from other instruments that operate in the similar energy range of 1-10 keV. Careful and detailed spectrum analysis shall be a necessary contribution to our future work - searching for axion-like particles' manifestations in the Coma cluster.

astro-ph.CO↗

arXiv2023

Spin exchange dynamics in 4H SiC monocrystals with different nitrogen donor concentrations

4H silicon carbide (SiC) polytype is preferred over other SiC polytypes for high-power, high-voltage, and high-frequency applications due to its superior electrical, thermal, and structural characteristics. In this manuscript, we provide a comprehensive study of the spin coupling dynamic between conduction electrons and nitrogen (N) donors in monocrystalline 4H SiC with various concentrations of uncompensated N donors from 10^17 cm^-3 to 5x10^19 cm^-3 by continuous wave, pulsed EPR, and microwave perturbation techniques at T=4.2-300 K. At low temperatures two triplets due to N donors in cubic (Nk) hexagonal (Nh) positions and triplet arisen from spin-interaction between Nh and Nk were observed in 4H SiC having Nd-Na=10^17 cm^-3. A single S-line (S=1/2) dominates the EPR spectra in all investigated 4H SiC monocrystals at high temperatures. It was established that this line occurs due to the exchange coupling of localized electrons (dominate at low temperatures) and non-localized electrons (dominate at high temperatures). The localized electrons were attributed to Nh for Nd-Na=10^17 cm^-3 and Nk donors for Nd-Na>=5x10^18 cm^-3. We have concluded that the conduction electrons in 4H SiC monocrystals are characterized by gpar=2.0053(3) gper=2.0011(3) for Nd-Na<=5x10^18 cm^-3 and gpar=2.0057(3) and gper=2.0019(3) for Nd-Na=5x10^19 cm^-3. Using the theoretical fitting of the temperature variation of S-line EPR linewidth in 4H SiC having Nd-Na<5x10^18 cm-^3, the energy levels of 57-65 meV that correlate with the valley-orbit splitting values for Nk donors in 4H SiC monocrystals were obtained.

cond-mat.mtrl-sci↗

arXiv2023

Neutrino signal from a population of Seyfert galaxies

IceCube collaboration has previously reported an evidence for neutrino signal from a Seyfert galaxy NGC 1068. This may suggest that all Seyfert galaxies emit neutrinos. To test this hypothesis, we identify the best candidate neutrino sources among nearby Seyfert galaxies, based on their hard X-ray properties. Only two other sources, NGC 4151 and NGC 3079 are expected to be detectable in 10 years of IceCube data. We find an evidence (~3 sigma)} for neutrino signal from both sources in publicly available ten-year IceCube dataset. {Though neither source alone is above the threshold for discovery,} the chance coincidence probability to find the observed neutrino count excesses in the directions of the two out of two expected sources, in addition to the previously reported brightest source, is p<2.6e-7. This corresponds to a correlation between Seyfert galaxies and neutrino emission.

astro-ph.HE↗

arXiv2023

Energy-dependent periodicities of LS I +61$^\circ$ 303 in the GeV band

LS I +61$^\circ$303 is a rare representative of the gamma-ray binaries with a compact object known to be a pulsar. We report on the periodicity and spectral analysis of this source performed with more than 14 years of Fermi/LAT data. The periodicity of LS I +61$^\circ$303 is strongly energy dependent. Two periods $P_1 = 26.932\pm 0.004 (stat)\pm 0.008 (syst)$ and $P_2 = 26.485 \pm 0.004 (stat)\pm 0.007 (syst)$ are detected only at $E>1$ GeV and at $E<0.3$ GeV correspondingly. Within $1\sigma$ (stat+syst) the periods are consistent with orbital ($P_2$) and beat orbital/superorbital ($P_1$) periods. We present the orbital light curves of the system in several energy bands and the results of the spectral analysis. We discuss the possible origin of the change in the variability pattern between 0.1 and 1 GeV energy.

astro-ph.HE↗

arXiv2019

New model of density distribution for fermionic dark matter halos

In this paper, we formulate a new model of density distribution for halos made of warm dark matter (WDM) particles. The model is described by a single microphysics parameter - the mass (or, equivalently, the maximal value of the initial phase-space density distribution) of dark matter particles. Given the WDM particle mass and the parameters of a dark matter density profile at the halo periphery, this model predicts the inner density profile. In case of initial Fermi-Dirac distribution, we successfully reproduce cored dark matter profiles from N-body simulations. Also, we calculate the core radii of warm dark matter halos of dwarf spheroidal galaxies for particle masses $m_\text{FD}=$100, 200, 300 and 400 eV.

astro-ph.GA↗

arXiv2019

Surface brightness profile of the 3.5 keV line in the Milky Way halo

We report a detection of 3.5 keV line in the Milky Way in 5 regions offset from the Galactic Center by distances from 10' to 35 degrees. We build an angular profile of this line and compare it with profiles of several astrophysical lines detected in the same observations. We compare our results with other detections and bounds previously obtained using observations of the Milky Way.

astro-ph.HE↗

arXiv2017

Local moment formation and magnetic coupling of Mn guest atoms in Bi$_2$Se$_3$: a low-temperature ferromagnetic resonance study

We compare the magnetic and electronic configuration of single Mn atoms in molecular beam epitaxy (MBE) grown Bi$_2$Se$_3$ thin films, focusing on electron paramagnetic (ferromagnetic) resonance (EPR and FMR, respectively) and superconducting quantum interference device (SQUID) techniques. X-ray diffraction (XRD) and electron backscatter diffraction (EBSD) reveal the expected increase of disorder with increasing concentration of magnetic guest atoms, however, Kikuchi patterns show that disorder consists majorly of mum-scale 60deg twin domains in the hexagonal Bi$_2$Se$_3$ structure, which are promoted by the presence of single unclustered Mn impurities. Ferromagnetism below T$_C$ ~ (5.4 +/- 0.3) K can be well described by critical scaling laws M(T) ~ (1-T/T$_C$)$^β$ with a critical exponent $β$ = (0.34 +/- 0.2)), suggesting 3D Heisenberg class magnetism instead of e.g. 2D-type coupling between Mn-spins in van der Waals gap sites. From EPR hyperfine structure data we determine a Mn$^{2+}$ (d$^5$, S = 5/2) electronic configuration with a g-factor of 2.002 for -1/2 --> +1/2 transitions. In addition, from the strong dependence of the low temperature FMR fields and linewidth on the field strength and orientation with respect to the Bi$_2$Se$_3$ (0001) plane, we derive magnetic anisotropy energies of up to K1 = -3720 erg/cm3 in MBE-grown Mn-doped Bi$_2$Se$_3$, reflecting the first order magneto-crystalline anisotropy of an in-plane magnetic easy plane in a hexagonal (0001) crystal symmetry. Across the ferromagnetic-paramagnetic transition the FMR intensity is suppressed and resonance fields converge the paramagnetic limit of a Mn$^{2+}$ (d$^5$, S = 5/2).

cond-mat.mtrl-sci↗

arXiv2016

The spin relaxation of nitrogen donors in 6H SiC crystals as studied by the electron spin echo method

We present the detailed study of the spin kinetics of the nitrogen (N) donor electrons in 6H SiC wafers grown by Lely method and by sublimation "sandwich method" (SSM) with a donor concentration of about 10^17 cm^-3 at T = 10-40 K. The donor electrons of the N donors substituting quasi-cubic "k1" and "k2" sites (Nk1,k2) in both types of the samples revealed the similar temperature dependence of the spin-lattice relaxation rate (T1^-1), which was described by the direct one-phonon and two-phonon processes induced by the acoustic phonons proportional to T and to T^9, respectively. The character of the temperature dependence of the T1^-1 for the donor electrons of N substituting hexagonal ("h") site (Nh) in both types of 6H SiC samples indicates that the donor electrons relax through the fast-relaxing centers by means of the cross-relaxation process. The observed enhancement of the phase memory relaxation rate (Tm^-1) with the temperature increase for the Nh donors in both types of the samples, as well as for the Nk1,k2 donors in Lely grown 6H SiC, was explained by the growth of the free electron concentration with the temperature increase and their exchange scattering at the N donor centers. The observed significant shortening of the phase memory relaxation time Tm for the Nk1,k2 donors in the SSM grown sample with the temperature lowering is caused by hopping motion of the electrons between the occupied and unoccupied states of the N donors at Nh and Nk1,k2 sites. The impact of the N donor pairs, triads, distant donor pairs formed in n-type 6H SiC wafers on the spin relaxation times was discussed.

cond-mat.mtrl-sci↗

arXiv2015

Temperature dependent behavior of localized and delocalized electrons in nitrogen-doped 6H SiC crystals as studied by electron spin resonance

We have studied the temperature behavior of the electron spin resonance (ESR) spectra of nitrogen (N) donors in n-type 6H SiC crystals grown by Lely and sublimation sandwich methods (SSM) with donor concentration of 10^17 cm^(-3) at T=60-150 K. A broad signal in the ESR spectrum was observed at T>=80 K with Lorentzian lineshape and gpar=2.0043(3), gper=2.0030(3), which was previously assigned in the literature to the N donors in the 1s(E) excited state. Based on the analysis of the ESR lineshape, linewidth and g-tensor we attribute this signal to the conduction electrons (CE). The emergence of the CE ESR signal at T>80 K was explained by the ionization of electrons from the 1s(A) ground and 1s(E) excited states of N donors to the conduction band while the observed reduction of the hyperfine (hf) splitting for the Nk1,k2 donors with the temperature increase is attributed to the motion narrowing effect of the hf splitting. The temperature dependence of CE ESR linewidth is described by an exponential law (Orbach process) with the activation energy corresponding to the energy separation between 1s(A1) and 1s(E) energy levels for N residing at quasi-cubic sites (Nk1,k2). The theoretical analysis of the temperature dependence of microwave conductivity measured by the contact-free method shows that due to the different position of the Fermi level in two samples the ionization of free electrons occurs from the energy levels of Nk1,k2 donors in Lely grown samples and from the energy level of Nh residing at hexagonal position in 6H SiC grown by SSM

cond-mat.mtrl-sci↗

arXiv2011

ESR and TSL study of hole capture in PbWO_4:Mo,La and PbWO_4:Mo,Y scintillator crystals

The processes of hole localization in double-doped PbWO_4:Mo,La and PbWO_4:Mo,Y single crystals have been studied by continuous wave and pulse electron spin resonance (ESR) and thermally stimulated luminescence (TSL) methods. We show that the holes created by the UV irradiation are preferably trapped at lattice oxygen ions in the vicinity of perturbing defects such as lead vacancies, impurity ions (La, Y, Mo), and other lattice imperfections. This leads to a variety of O^- centers, which differ both by thermal stability (from about 170 K up to 240 K) and ESR parameters. The hole centers of this type were not observed neither in PbWO_4:Mo nor in PbWO_4:La(Y) crystals. The recombination processes of thermally released holes with electrons stored at different traps, including Pb^+ - WO_3 and (MoO_4)^3- centers, are systematically studied by TSL. Thermal stability parameters are defined by ESR and TSL techniques for different O^- type defects.

cond-mat.mtrl-sci↗