Low Relative Velocities Research Articles

Collisions of dark matter axion stars with astrophysical sources

If QCD axions form a large fraction of the total mass of dark matter, then axion stars could be very abundant in galaxies. As a result, collisions with each other, and with other astrophysical bodies, can occur. We calculate the rate and analyze the consequences of three classes of collisions, those occurring between a dilute axion star and: another dilute axion star, an ordinary star, or a neutron star. In all cases we attempt to quantify the most important astrophysical uncertainties; we also pay particular attention to scenarios in which collisions lead to collapse of otherwise stable axion stars, and possible subsequent decay through number changing interactions. Collisions between two axion stars can occur with a high total rate, but the low relative velocity required for collapse to occur leads to a very low total rate of collapses. On the other hand, collisions between an axion star and an ordinary star have a large rate, Γ⊙ ∼ 3000 collisions/year/galaxy, and for sufficiently heavy axion stars, it is plausible that most or all such collisions lead to collapse. We identify in this case a parameter space which has a stable region and a region in which collision triggers collapse, which depend on the axion number (N ) in the axion star, and a ratio of mass to radius cubed characterizing the ordinary star (Ms/Rs3). Finally, we revisit the calculation of collision rates between axion stars and neutron stars, improving on previous estimates by taking cylindrical symmetry of the neutron star distribution into account. Collapse and subsequent decay through collision processes, if occurring with a significant rate, can affect dark matter phenomenology and the axion star mass distribution.

Revisiting the collision risk with cataloged objects for the Iridium and COSMO-SkyMed satellite constellations

After two decades of slightly declining growth rate, the population of cataloged objects around the Earth increased by more than 56% in just a couple of years, from January 2007 to February 2009, due to two collisions in space involving the catastrophic destruction of three intact satellites (Fengyun 1C, Cosmos 2251 and Iridium 33) in high inclination orbits. Both events had occurred in the altitude range already most affected by previous launch activity and breakups. In 2011 a detailed analysis had been carried out to analyze the consequences of these fragmentations, in particular concerning the evolution of the collision risk for the Iridium and COSMO-SkyMed satellite constellations. Five years after such first assessment, the cataloged objects environment affecting the two constellations was revisited to evaluate how the situation had evolved due to the varying contribution of the above mentioned breakup fragments and the space activities carried out in the meantime. Being distributed, at 778km, over six nearly polar orbit planes separated by just 30° at the equator, the Iridium satellites represent a very good gauge for checking the evolution of the environment in the most critical low Earth region. In approximately five years, from May 2011 to June 2016, the average flux of cataloged objects on the Iridium satellites increased by about 14%, to 1.59×10−5m−2 per year. The cataloged fragments of Fengyun 1C, Cosmos 2251 and Iridium 33 still accounted for, on average, 54% of the total flux. More than 39% of the latter was associated with the Fengyun 1C fragments, about 11% with the Cosmos 2251 fragments and less than 4% with the Iridium 33 fragments. Specifically concerning the mutual interaction among the Iridium 33 debris and the parent constellation, the progressive dispersion and rather fast decay of the fragments below the Iridium operational altitude, coupled with a slow differential plane precession and low average relative velocities with respect to four of the six constellation planes, determined in five years, on average, a decline of the flux by about 31%, i.e. to about 5.75×10−7m−2 per year. The decrease occurred in each constellation plane, even though with different rates and percentages, due to the varying relative orbit geometry. From May 2011 to June 2016, the mean flux of cataloged objects on the COSMO-SkyMed satellites, at 623km, increased by about 26%, to 7.24×10−6m−2 per year. The Fengyun 1C, Cosmos 2251 and Iridium 33 cataloged fragments accounted for, on average, about 1/4 of the total, with 12% due to Fengyun 1C, 8% to Cosmos 2251 and 4% to Iridium 33.

The closest quasi-satellite to Earth

Celestial Mechanics A quasi-satellite orbits close to a planet, circling the Sun with the same orbital period, but it is not gravitationally bound to the planet. The fifth known quasi-satellite of Earth was discovered earlier this year: an asteroid with the snappy name (469219) 2016 HO3. In a recent study, de la Fuente Marcos and de la Fuente Marcos investigated its orbit with numerical simulations, showing that it will remain an Earth quasi-satellite for a few centuries. The asteroid, which is a few dozen meters across, stays between 38 and 100 times as far away from Earth as the Moon. This proximity and its low relative velocity make the object a tempting target for a visit by a sample-return mission—or even by astronauts. Mon. Not. R. Astron. Soc. 10.1093/mnras/stw1972 (2016).

Electron–positron pair production in ion collisions at low velocity beyond Born approximation

We derive the spectrum and the total cross section of electromagnetic $e^{+}e^{-}$ pair production in the collisions of two nuclei at low relative velocity $\beta$. Both free-free and bound-free $e^{+}e^{-}$ pair production is considered. The parameters $\eta_{A,B}=Z_{A,B}\alpha$ are assumed to be small compared to unity but arbitrary compared to $\beta$ ($Z_{A,B}$ are the charge numbers of the nuclei and $\alpha$ is the fine structure constant). Due to a suppression of the Born term by high power of $\beta$, the first Coulomb correction to the amplitude appears to be important at $\eta_{A,B}\gtrsim \beta$. The effect of a finite nuclear mass is discussed. In contrast to the result obtained in the infinite nuclear mass limit, the terms $\propto M^{-2}$ are not suppressed by the high power of $\beta$ and may easily dominate at sufficiently small velocities.

Analytical study of the end-face friction loss in a synchronal rotary multiphase pump

This study introduces a new type of end-face structure with polytetrafluoroethylene seals that improves the reliability of the synchronal rotary multiphase pump (SRMP). End-face models, including the relative motion and friction loss between the rotor and cylinder end faces, are established for both the original and the improved end-face structures. The end-face friction losses are analytically investigated based on the theoretical calculations. Due to the low relative velocity between the rotor and cylinder end faces, the end-face friction losses for both of the end-face structures are found to be insignificant compared to the total friction loss in the SRMP. The increased end-face friction loss caused by the polytetrafluoroethylene seals in the improved end-face structure is also negligible. Assessment of the friction losses of two end-face structures in high-speed and high-pressure applications shows that the improved end-face structure exhibits better performance than the original. The parametric analysis suggests that the wider but taller cylinder is helpful in reducing the end-face friction loss of SRMP.

Typology of dust particles collected by the COSIMA mass spectrometer in the inner coma of 67P/Churyumov Gerasimenko

The COSIMA mass spectrometer on board the ROSETTA orbiter has collected dust in the near coma of comet 67P/Churyumov-Gerasimenko since August 11, 2014. The collected dust particles are identified by taking images with a microscope (COSISCOPE) under grazing incidence illumination before and after exposure of the target to cometary dust. More than 10,000 dust particles >14 µm in size collected from August 11, 2014 to April 3, 2015 have been detected on three distinct target assemblies, including ∼500 dust particles with sizes ranging from 50 to more than 500 µm, that can be resolved by COSISCOPE (pixel size 14 µm). During this period, the heliocentric distance decreased from 3.5 AU to less than 2 AU. The collection efficiency on targets covered with “metal black” has been very high, due to the low relative velocity of incoming dust. Therefore, the COSISCOPE observations provide the first optical characterization of an unbiased sample of particles collected in the inner coma of a comet. The typology of particles >100 µm in size is dominated by clusters with a wide range of structure and strength, most originating from the disruption of large aggregates (>1 mm in size) shortly before collection. A generic relationship between these clusters and IDPs/Antarctic meteorites is likely in the framework of accretion models. About 15% of particles larger than 100 µm are compact particles with two likely contributions, one being linked to clusters and another leaving the cometary nucleus as single compact particles.

Dark-matter bound states from Feynman diagrams

If dark matter couples directly to a light force mediator, then it may form bound states in the early universe and in the non-relativistic environment of haloes today. In this work, we establish a field-theoretic framework for the computation of bound-state formation cross-sections, de-excitation and decay rates, in theories with long-range interactions. Using this formalism, we carry out specific computations for scalar particles interacting either via a light scalar or vector mediator. At low relative velocities of the interacting particles, the formation of bound states is enhanced by the Sommerfeld effect. For particle-antiparticle pairs, we show that bound-state formation can be faster than annihilation into radiation in the regime where the Sommerfeld effect is important. The field-theoretic formalism outlined here can be generalised to compute bound-state formation cross-sections in a variety of theories, including theories featuring non-Abelian (albeit non-confining) interactions, such as the electroweak interactions.

Anisotropic diffusion of volatile pollutants at air-water interface

The volatile pollutants that spill into natural waters cause water pollution. Air pollution arises from the water pollution because of volatilization. Mass exchange caused by turbulent fluctuation is stronger in the direction normal to the air-water interface than in other directions due to the large density difference between water and air. In order to explore the characteristics of anisotropic diffusion of the volatile pollutants at the air-water interface, the relationship between velocity gradient and mass transfer rate was established to calculate the turbulent mass diffusivity. A second-order accurate smooth transition differencing scheme (STDS) was proposed to guarantee the boundedness for the flow and mass transfer at the air-water interface. Simulations and experiments were performed to study the trichloroethylene (C2HCl3) release. By comparing the anisotropic coupling diffusion model, isotropic coupling diffusion model, and non-coupling diffusion model, the features of the transport of volatile pollutants at the air-water interface were determined. The results show that the anisotropic coupling diffusion model is more accurate than the isotropic coupling diffusion model and non-coupling diffusion model. Mass transfer significantly increases with the increase of the air-water relative velocity at a low relative velocity. However, at a higher relative velocity, an increase in the relative velocity has no effect on mass transfer.

PLANET FORMATION IN STELLAR BINARIES. I. PLANETESIMAL DYNAMICS IN MASSIVE PROTOPLANETARY DISKS

About $20\%$ of exoplanets discovered by radial velocity surveys reside in stellar binaries. To clarify their origin one has to understand the dynamics of planetesimals in protoplanetary disks within binaries. The standard description, accounting for only gas drag and gravity of the companion star has been challenged recently, as the gravity of the protoplanetary disk was shown to play a crucial role in planetesimal dynamics. An added complication is the tendency of protoplanetary disks in binaries to become eccentric, giving rise to additional excitation of planetesimal eccentricity. Here, for the first time, we analytically explore secular dynamics of planetesimals in binaries such as $\alpha$ Cen and $\gamma$ Cep under the combined action of (1) gravity of the eccentric protoplanetary disk, (2) perturbations due to the (coplanar) eccentric companion, and (3) gas drag. We derive explicit solutions for the behavior of planetesimal eccentricity ${\bf e}_p$ in non-precessing disks (and in precessing disks in certain limits). We obtain the analytical form of the distribution of relative velocities of planetesimals, which is a key input for understanding their collisional evolution. Disk gravity strongly influences relative velocities and tends to push sizes of planetesimals colliding with comparable objects at the highest speed to small values, $\sim 1$ km. We also find that planetesimals in eccentric protoplanetary disks apsidally aligned with the binary orbit collide at lower relative velocities than in mis-aligned disks. Our results highlight a decisive role that disk gravity plays in planetesimal dynamics in binaries.

Experimental results on the flow rheology of fiber-laden aqueous foams

Abstract We report here the first experimental results on the rheology of fiber-laden aqueous foams. The measurements were carried out in a laboratory-scale environment with a glass pipe of diameter 15 mm. The slip velocity at the pipe wall was measured with high-speed video imaging. Plain aqueous foam was generated from 8.5 mM aqueous solution of sodium dodecyl sulphate (SDS). Foam generation was realized as a combination of tank mixing and injection of compressed air in a special inline generation block (turbulence generator) installed into the flow loop. Fiber-laden foam was prepared by dispersing hardwood fibers into the SDS solution at consistency of 20 g/kg. In the measurements, an absolute slip velocity was observed that increased with the wall shear stress. On the other hand, the relative slip velocity decreased with the wall shear stress. At highest shear stresses relative slip values of ca. 10% were observed, i.e. considerable shearing took place inside the foam. At low wall shear stress relative slip velocities up to 40% were measured. The addition of wood fibers decreased the absolute slip by ca. 25% while the relative slip increased by a factor close to four. The real wall shear rate in foam was calculated with the Weissenberg–Rabinowitsch correction. All the studied foams could be modeled with Herschel–Bulkley law with flow behavior index n = 0.5. The viscosity of the fiber-laden foam was ca. 100% larger than that of the plain aqueous foam at same density and temperature. This increase in viscosity is much less than in the case of plain aqueous fiber suspension, where the viscosity increases by a factor five or more due to fibers being in continuous contact in shearing. Thus the current results imply that in aqueous foams fibers do not interact or flocculate to the same extent as in plain aqueous suspensions. By applying the methodology described here on the data measured with one pipe diameter, one can calculate real material properties that are independent of boundary effects like slip velocity.

3-D laser images of splash-form tektites and their use in aerodynamic numerical simulations of tektite formation

Ten splash-form tektites from the Australasian strewn field, with masses ranging from 21.20 to 175.00 g and exhibiting a variety of shapes (teardrop, ellipsoid, dumbbell, disk), have been imaged using a high-resolution laser digitizer. Despite challenges due to the samples’ rounded shapes and pitted surfaces, the images were combined to create 3-D tektite models, which captured surface features with a high fidelity (≈30 voxel mm−2) and from which volume could be measured noninvasively. The laser-derived density for the tektites averaged 2.41 ± 0.11 g cm−3. Corresponding densities obtained via the Archimedean bead method averaged 2.36 ± 0.05 g cm−3. In addition to their curational value, the 3-D models can be used to calculate the tektites’ moments of inertia and rotation periods while in flight, as a probe of their formation environment. Typical tektite rotation periods are estimated to be on the order of 1 s. Numerical simulations of air flow around the models at Reynolds numbers ranging from 1 to 106 suggest that the relative velocity of the tektites with respect to the air must have been <10 m s−1 during viscous deformation. This low relative velocity is consistent with tektite material being carried along by expanding gases in the early time following the impact.

Sex-Specific Responses to Self-Paced, High-Intensity Interval Training With Variable Recovery Periods

This study examined sex-specific responses during self-paced, high-intensity interval training (HIIT). Sixteen (8 men and 8 women) individuals completed a peak oxygen uptake test and 3 treadmill HIIT sessions on separate days. The HIIT sessions consisted of six 4-minute intervals performed at the highest self-selected intensity individuals felt they could maintain. Recovery between intervals was counterbalanced and consisted of 1-, 2-, or 4-minute recovery during each trial. Relative measures of intensity, including percentage of velocity at VO2peak (vVO2peak), %VO2peak, %HRmax, and blood lactate concentration ([La]), were observed during the trials. Perceived readiness was recorded immediately before and ratings of perceived exertion (RPE) were recorded at the end of each interval with session RPE recorded after each trial. Results revealed a significant effect of sex on %vVO2peak (p < 0.01) and %HRmax (p < 0.01). Data show that across trials, men self-select higher %vVO2peak (84.5 vs. 80.7%), whereas women produce higher %HRmax (96.9 vs. 92.1%) and %VO2peak (89.6 vs. 86.1%) with no difference in [La] or perceptual responses. These findings support the notion that women may demonstrate improved recovery during high-intensity exercise, as they will self-select intensities resulting in greater cardiovascular strain. Moreover, results confirm previous findings suggesting that a 2:1 work-to-rest ratio is optimal during HIIT for both men and women.

STELLAR KINEMATICS AND STRUCTURAL PROPERTIES OF VIRGO CLUSTER DWARF EARLY-TYPE GALAXIES FROM THE SMAKCED PROJECT. I. KINEMATICALLY DECOUPLED CORES AND IMPLICATIONS FOR INFALLEN GROUPS IN CLUSTERS

We present evidence for kinematically decoupled cores (KDCs) in two dwarf early-type (dE) galaxies in the Virgo cluster, VCC 1183 and VCC 1453, studied as part of the SMAKCED stellar absorption-line spectroscopy and imaging survey. These KDCs have radii of 1.8'' (0.14 kpc) and 4.2'' (0.33 kpc), respectively. Each of these KDCs is distinct from the main body of its host galaxy in two ways: (1) inverted sense of rotation; and (2) younger (and possibly more metal-rich) stellar population. The observed stellar population differences are probably associated with the KDC, although we cannot rule out the possibility of intrinsic radial gradients in the host galaxy. We describe a statistical analysis method to detect, quantify the significance of, and characterize KDCs in long-slit rotation curve data. We apply this method to the two dE galaxies presented in this paper and to five other dEs for which KDCs have been reported in the literature. Among these seven dEs, there are four significant KDC detections, two marginal KDC detections, and one dE with an unusual central kinematic anomaly that may be an asymmetric KDC.The frequency of occurence of KDCs and their properties provide important constraints on the formation history of their host galaxies. We discuss different formation scenarios for these KDCs in cluster environments and find that dwarf-dwarf wet mergers or gas accretion can explain the properties of these KDCs. Both of these mechanisms require that the progenitor had a close companion with a low relative velocity. This suggests that KDCs were formed in galaxy pairs residing in a poor group environment or in isolation whose subsequent infall into the cluster quenched star formation.

Y- and T-junction microfluidic devices: effect of fluids and interface properties and operating conditions

Water-in-oil emulsions were produced in microchannels with Y- and T-junction geometries by individual droplet generation. For each microchannel configuration, the effect of the fluids and interface properties as well as of the process conditions was evaluated. The size of the droplets depended mainly on the relative velocity between continuous and dispersed phases and the relative fluid viscosity between phases. Those variables were related to the shear stress between the phases, which caused the droplet detachment. In addition, the interfacial forces played a minor role in Y-junction, and they had no effect in the droplets formation in T-junction microchannels. In Y-junction, a large variation in the droplet size was observed, depending on the system composition and the operating conditions. At low relative velocity and fluid viscosity, no droplets were generated. In contrast, the process in T-junction resulted in a lower variation of droplets size and the droplets were formed even at less favorable conditions. Such results indicate that the knowledge of the mechanism of droplets generation in each microchannel geometry makes it possible to choose the appropriate configuration according to the type of fluid, and the operating conditions can be adjusted to obtain the desired final emulsion.

Gamma-Ray Effects of Dark Forces in Dark Matter Clumps

Existence of new gauge U(1) symmetry possessed by dark matter (DM) particles implies the existence of a new Coulomb-like interaction, which leads to Sommerfeld-Gamow-Sakharov enhancement of dark matter annihilation at low relative velocities. We discuss a possibility to put constraints on such dark forces of dark matter from the observational data on the gamma radiation in our Galaxy. Gamma-rays are supposed to originate from annihilation of DM particles in the small scale clumps, in which annihilation rate is supposed to be enhanced, besides higher density, due to smaller relative velocitiesvof DM particles. For possible cross sections, mass of annihilating particles, masses of clumps, and the contribution of annihilating particles in the total DM density we constrain the strength of new dark long range forces from comparison of predicted gamma-ray signal with Fermi/LAT data on unidentified point-like gamma-ray sources (PGS) as well as on diffuseγ-radiation. Both data on diffuse radiation and data on PGS put lower constraints on annihilation cross section at any dark interaction constant, where diffuse radiation provides stronger constraint at smaller clump mass. Density of annihilating DM particles is conventionally supposed to be defined by the frozen annihilation processes in early Universe.

Microbubble-Enhanced Cell Membrane Permeability in High Gravity Field

Cell permeability controls the transportation of extracellular materials through cell membranes, which plays a critical role in drug and gene delivery. This work reports an innovative method to enhance the cell permeability through cell-bubble interactions in a high gravity field. In the presence of microbubbles, the cell membrane permeability of mammalian cells was significantly increased in the high gravity field, and up to 80% THP-1 and 70% MCF-7 cells were permeabilized by using FITC-Dextran with average molecular weight of 40 and 70 kDa as fluorescent markers which were found to locate in both cytoplasm and cell nucleus by using a confocal microscope. Micro-scale pores were detected on the cell membrane by a scanning electron microscope after the cell-microbubble interactions in the high gravity field. The delivery efficiency of FITC-Dextran could be further enhanced in gravity field of higher strength and in solutions with higher volume fraction of microbubbles, though the cell viability would also fall under extreme conditions. A simplified model was proposed to compare the contributions of surface forces (i.e., Derjaguin–Landau–Verwey–Overbeek (DLVO) interaction force and membrane undulation force) with hydrodynamic force associated with cell-bubble interactions in the high gravity field. The hydrodynamic force was found to dominate the cell-bubble interaction while the DLVO force and membrane undulation force only play an important role at small separation (<10 nm) and low relative velocity of approach (i.e., low gravity field strength). The enhanced cell membrane permeability and formation of micro-scale pores are mainly due to the microbubble-cell interactions through collision and/or cavitation effects from the bursting of microbubbles. Our results have important implications in many bioengineering processes which are dependent on cell membrane permeability.

Turbulence-induced collision velocities and rates between different sized dust grains

We study the collision rates and velocities for point-particles of different sizes in turbulent flows. We construct fits for the collision rates at specified velocities (effectively a collisional velocity probability distribution) for particle stopping time ratios up to four; already by that point the collisional partners are very poorly correlated and so the results should be robust for even larger stopping time ratios. Significantly, we find that while particles of very different masses have approximately Maxwellian collisional statistics, as the mass ratio shrinks the distribution changes dramatically. At small stopping time ratios, the collisional partners are highly correlated and we find a population of high number density (clustered), low relative-velocity particle pairs. Unlike in the case of identical stopping time collisional partners, this low relative-velocity clustered population is collisional, but the clustering is barely adequate to trigger bulk effects such as the streaming instability. We conclude our analysis by constructing a master fit to the collisional statistics as a function only of the stopping time ratio. Together with our previous work for identical stopping time particle pairs, this provides a recipe for including collisional velocity probability distributions in dust coagulation models for protoplanetary disks. We also include our recipe for determining particle collisional diagnostics from numerical simulations.

Relative Motion Between the Rivera and North American Plates Determined from the Slip Directions of Earthquakes

So far, the direction and rate of relative motion between the Rivera and the North American plates (RIV-NAM) has been determined by the combination of two Euler poles: Rivera (RIV), with respect to Pacific (PAC), and PAC with respect to North America. Here, we estimate the relative motion of this plate pair (RIV-NAM) assuming that the horizontal projection of the direction of slip of the earthquakes occurring on the RIV-NAM boundaries reflect their relative plate motion. A catalog of earthquakes for which focal mechanisms are reported since 1976 is used in the analysis. Earthquakes were considered in the three segments of the RIV-NAM plate boundary: the subduction zone of the Rivera plate beneath the Jalisco block, the Tres Marias Escarpment and the events associated with the Tamayo Fracture Zone. The best fitting Euler pole is determined using a grid search of 64 potential poles. The slip direction predicted for each grid point is compared to the slip direction of the focal mechanisms of the earthquakes on the plate boundary. The best fitting Euler pole, determined in a root mean square sense (RMS), is located at 21.8°N, 107.6°W. A rate of rotation of 5.3°/year is estimated assuming the seismic earthquake cycle of the 1932 and 1995 great earthquakes represents a lower bound of the rate of plate motion in the subduction zone. The best fitting Euler pole shows that the subduction of the Rivera plate takes place in a direction perpendicular to the trench with a relative velocity of 4.3 cm/year, offshore Manzanillo. The rate of relative motion RIV-NAM decreases from SE to NW. North of approximately 21°N, the subduction of the Rivera plate becomes oblique to the trench and the relative velocity between the two plates decreases to an average of 1.9 cm/year. This slow rate of convergence may explain the rapid decrease of seismicity in the trench and the apparent absence of large earthquakes in this region. In the Tres Marias Escarpment, our best-fitting pole suggests that subduction stops, giving way to high-angle reverse faulting perpendicular to the Tres Marias Escarpment, in agreement with the reverse faulting earthquakes occurring here. To the north of 22.5°N, the slip predicted by the best-fitting pole suggests right-lateral faulting in a direction parallel to the Tamayo Fracture Zone, at a very low velocity (0.5–1.0 cm/year). The best fitting Euler pole determined here lies very close to the RIV-NAM plate boundary in the vicinity of the Tamayo Fracture Zone. This location of our best fitting Euler pole explains the low relative plate velocity, the relatively low level of seismic activity and the presence of a broad zone of deformation that accommodates the RIV-NAM motion.

Astrophysical manifestations of clumps of cold dark matter

Small-scale structures (clumps) of dark matter may manifest themselves owing to the annihilation of dark-matter particles in them as pointlike gamma-ray sources. In view of this, investigation into respective effects on the basis of data on unidentified pointlike gamma-ray sources is of importance. It is shown that the existing uncertainties in the description of physical properties of dark-matter particles (their annihilation cross section) and in the distribution of their density in the clumps are of crucial importance; therefore, an analysis of data from the observation of pointlike gamma-ray sources makes it possible to impose constraints on the values of respective uncertain parameters (that is, to single out preferable ones). It is considered that the rate of annihilation of dark-matter particles in the clumps may be enhanced both owing to a higher density and owing to the growth of the cross section at low relative velocities of dark-matter particles in the clumps. In particular, dark-matter particles may have self-interaction of the Coulomb type, and this leads to the enhancement of the annihilation rate because of the Sommerfeld-Sakharov effect. It is shown that the heavy-neutrino model featuring an extra interaction can explain partly Fermi and EGRET data on unidentified pointlike gamma-ray sources. It is indicated that the motion of gamma-ray sources over the celestial sphere can be noticed for several clumps within several years of observations.

아리랑 위성들의 경향에 따른 및 3차원 충돌확률 분석

우주파편과의 위험성을 판단하는데 가장 보편적으로 사용되는 것이 충돌확률이며, 현재 널리 사용되고 있는 방법은 최근접거리를 이용한 2차원 선형 충돌확률 계산방법이다. 본 논문에서는 우리나라가 운용하거나 운용을 계획 중인 아리랑 2호, 3호, 5호 위성에 접근하는 물체의 접근 특성을 분석하고, 2차원 선형 충돌확률보다 더 정밀한 3차원 비선형 충돌확률의 특성을 STK/Nonlinear Collision Probability Tool을 이용하여 분석하였다. 이를 통해 저궤도 위성인 아리랑 위성들에 대해 3차원 비선형 충돌확률의 효용성에 대해 고찰하였다. 분석결과 3차원 비선형 충돌확률은 350m/s 이하의 상대속도 영역에서 효용성이 있음을 확인하였으며, 우리나라 위성의 경우 낮은 상대속도를 가지고 접근하는 경우가 거의 없는 것으로 나타나 실질적으로 3차원 비선형 충돌확률에 대한 효용성이 낮은 것으로 나타났다. Collision probability is the most common method to measure the risk of space debris, it is widely used that two dimensional linear collision probability using the closest approach distance. This paper represents the characteristics of object that approach KOMPSAT 2, 3, 5 that have operated or will be operated by Korea. And more precise method than two dimensional linear collision probability, we analyzed the properties of three dimensional nonlinear collision probability using STK/Nonlinear Collision Probability Tool. Through this, efficiency of three dimensional nonlinear collision probability for KOMPSAT series satellites was investigated. The result represents that three dimensional nonlinear collision probability showed the precise outcome at a relative velocity of less than 350m/s. Also, KOMPSAT series satellites appeared to few low relative velocity approaches and showed low efficiency for the three dimensional nonlinear collision probability.