Terahertz imaging of sub-wavelength particles with Zenneck surface waves

Impact of sub-wavelength-size dielectric particles on Zenneck surface waves on planar metallic antennas is investigated at terahertz (THz) frequencies with THz near-field probe microscopy. Perturbations of the surface waves show the particle presence, despite its sub-wavelength size. The experimental configuration, which utilizes excitation of surface waves at metallic edges, is suitable for THz imaging of dielectric sub-wavelength size objects. As a proof of concept, the effects of a small strontium titanate rectangular particle and a titanium dioxide sphere on the surface field of a bow-tie antenna are experimentally detected and verified using full-wave simulations

Are Slope Streaks Indicative of Global-Scale Aqueous Processes on Contemporary Mars?

Acknowledgments We acknowledge the editorial board of Reviews of Geophysics for inviting the submission of this review article. We extend our gratitude to the efforts of the handling editor and the reviewers. We thank NASA, JPL‐Caltech, JPL/Goddard, University of Arizona, Malin Space Science systems, Arizona State University, USGS, ESA/DLR/FU Berlin, and Google Earth for providing various satellite images, maps, and JMARS software free of charge. The paper is theoretical, and no new data have been generated during the work. All the used satellite images of Mars can be rendered on JMARS software using the image ID provided in the respective figure captions, and the image sources have also been duly acknowledged in the respective figure captions. The maps in various figures have been created using ArcGIS version 10.4 (http://desktop.arcgis.com/en/arcmap/latest/get‐started/setup/arcgis‐desktop‐quick‐start‐guide.htm). Although we have cited all the previous research results used in the paper, we here acknowledge the efforts of all those researchers in providing the essential inputs for our study. A. B. acknowledges the Swedish Research Council for supporting his research in cold arid environments. L. S. acknowledges the German Academic Exchange Service (DAAD) for her PhD scholarship.Peer reviewedPublisher PD

Graviton Production By Two Photon and Electron-Photon Processes In Kaluza-Klein Theories With Large Extra Dimensions

We consider the production of gravitons via two photon and electron-photon fusion in Kaluza-Klein theories which allow TeV scale gravitational interactions. We show that at electron-positron colliders, the processes l+l- -> l+ l- graviton, with l=e, mu, can lead to a new signal of low energy gravity of the form l+l- -> l+l- + missing energy which is well above the Standard Model background. For example, with two extra dimensions at the Next Linear Collider with a center of mass energy of 500 or 1000 GeV, hundreds to thousands such l+ l- graviton events may be produced if the scale of the gravitational interactions, M_D, is around a few TeV. At a gamma-electron collider, more stringent bounds may be placed on M_D via the related reaction e^-\gamma -> e^- graviton. For instance, if a 1TeV electron positron collider is converted to an electron-photon collider, a bound of ~10TeV may be placed on the scale M_D if the number of extra dimensions delta=2 while a bound of ~4TeV may be placed if delta=4.Comment: 25 pages 6 figures, minor changes made in the text and changes in reference

Resonant Cyclotron Radiation Transfer Model Fits to Spectra from Gamma-Ray Burst GRB870303

We demonstrate that models of resonant cyclotron radiation transfer in a strong field (i.e. cyclotron scattering) can account for spectral lines seen at two epochs, denoted S1 and S2, in the Ginga data for GRB870303. Using a generalized version of the Monte Carlo code of Wang et al. (1988,1989b), we model line formation by injecting continuum photons into a static plane-parallel slab of electrons threaded by a strong neutron star magnetic field (~ 10^12 G) which may be oriented at an arbitrary angle relative to the slab normal. We examine two source geometries, which we denote "1-0" and "1-1," with the numbers representing the relative electron column densities above and below the continuum photon source plane. We compare azimuthally symmetric models, i.e. models in which the magnetic field is parallel to the slab normal, with models having more general magnetic field orientations. If the bursting source has a simple dipole field, these two model classes represent line formation at the magnetic pole, or elsewhere on the stellar surface. We find that the data of S1 and S2, considered individually, are consistent with both geometries, and with all magnetic field orientations, with the exception that the S1 data clearly favor line formation away from a polar cap in the 1-1 geometry, with the best-fit model placing the line-forming region at the magnetic equator. Within both geometries, fits to the combined (S1+S2) data marginally favor models which feature equatorial line formation, and in which the observer's orientation with respect to the slab changes between the two epochs. We interpret this change as being due to neutron star rotation, and we place limits on the rotation period.Comment: LaTeX2e (aastex.cls included); 45 pages text, 17 figures (on 21 pages); accepted by ApJ (to be published 1 Nov 1999, v. 525

ПАЛЕОПРОТЕРОЗОЙСКАЯ ИМАНДРА-ВАРЗУГСКАЯ РИФТОГЕННАЯ СТРУКТУРА (КОЛЬСКИЙ ПОЛУОСТРОВ): ИНТРУЗИВНЫЙ МАГМАТИЗМ И МИНЕРАГЕНИЯ

The article provides data on the structure of the Paleoproterozoic intercontinental Imandra-Varzuga rifting structure (IVS) and compositions of intrusive formations typical of the early stage of the IVS development and associated mineral resources. IVS is located in the central part of the Kola region. Its length is about 350 km, and its width varies from 10 km at the flanks to 50 km in the central part. IVS contains an association of the sedimentary-volcanic, intrusive and dyke complexes. It is a part of a large igneous Paleoproterozoic province of the Fennoscandian Shield spreading for a huge area (about 1 million km2), which probably reflects the settings of the head part of the mantle plume. Two age groups of layered intrusions were associated with the initial stage of the IVS development. The layered intrusions of the Fedorovo-Pansky and Monchegorsk complexes (about 2.50 Ga) are confined to the northern flank and the western closure of IVS, while intrusions of the Imandra complex (about 2.45 Ga) are located at the southern flank of IVS. Intrusions of older complexes are composed of rock series from dunite to gabbro and anorthosites (Monchegorsk complex) and from orthopyroxenite to gabbro and anorthosites (Fedorovo-Pansky complex). Some intrusions of this complexes reveal features of multiphase ones. The younger Imandra complex intrusions (about 2.45 Ga) are stratified from orthopyroxenite to ferrogabbro. Their important feature is comagmatical connection with volcanites. All the intrusive complexes have the boninite-like mantle origin enriched by lithophyle components. Rocks of these two complexеs with different age have specific geochemical characteristics. In the rocks of the Monchegorsk and Fedorovo-Pansky complexes, the accumulation of REE clearly depends on the basicity of the rocks, the spectrum of REE is non-fractionated and ‘flat’, and the Eu positive anomaly is slightly manifested. In the rocks of the Imandra complex, the level of REE accumulation is relatively higher. The spectrum of REE here differs with more fractionated LREE with a ‘flat’ distribution of HREE and distinct Eu anomalies. Rocks of all the intrusive complexes are characterized mostly by negative eNd(T) values, and eNd values are distributed more heterogeneously in the rocks of the Monchegorsk complex than in the rocks of the Fedorovo-Pansky complex. Deposits and occurrences of Cr, complex PGE-Cu-Ni and low-sulfide Pt-Pd ores of the world class are spatially related and genetically associated with the IVS intrusive complexes. The Sopcheozero deposit (Monchepluton of the Monchegorsk complex) and Bolshaya Varaka deposit (the same-name intrusion of the Imandra complex) represent a layered Cr mineralization. Complex PGE-Cu-Ni deposits are confined to Monchepluton. They occur in vein ores of the Nittis-Kumuzhya-Travyanaya massifs (which have been worked out) and Sopcha, vein PGE-Cu, injecting Ni ores mostly and bottom deposits of the Nittis-Kumuzhya-Travyanaya massifs, as well as in the Nyud ‘critical’ horizon. In the past 10–15 years, low-sulphide Pt-Pd ores were discovered as new for the Kola region. Two main types of such ores have been distinguished: (1) stratiform (rift) ores being consistent with the massifs’ layering, and (2) basal ores located within lower marginal zones. Deposits of Kievey (West-Pansky massif of the Fedorovo-Pansky complex), horizon 330 of the Sopcha and Vurechuayvench (Monchepluton of the Monchegorsk complex) belong to the first type; the second type is represented by the Fedorovotundrovskoe (Fedorovo-Pansky complex), South Sopcha and Loypishnyun (Mon­chetundrovsky massif of Monchegorsk complex) deposits.   В статье приведены данные о строении палеопротерозойской внутриконтинентальной Имандра-Варзуг­ской рифтогенной структуры (ИВС), составе интрузивных образований ее раннего этапа развития и связанных с ними полезных ископаемых. ИВС расположена в центральной части Кольского региона, имеет протяженность около 350 км и ширину от 10 км на флангах до 50 км в центральной части и включает ассоциацию осадочно-вулканоген­ных, интрузивных и дайковых комплексов. Она входит в состав обширной изверженной палеопротерозойской провинции Фенноскандинавского щита, которая охватывает огромный площадной ареал развития (около 1 млн км2), отражающий, по-видимому, параметры головной части мантийного плюма. С начальным этапом развития ИВС свя­зано формирование двух возрастных групп расслоенных интрузий. К северному борту и западному замыканию структуры приурочены расслоенные интрузии Федорово-Панского и Мончегорского комплексов с возрастом около 2.50 млрд лет, а к южному борту структуры – интрузии Имандровского комплекса с возрастом около 2.45 млрд лет. Интрузии более древних комплексов образованы рядом пород от дунитов до габбро и анортозитов (Мончегорский комплекс) и от ортопироксенитов до габбро и анортозитов (Федорово-Панский комплекс). При этом в некоторых интрузиях этих комплексов установлены признаки их многофазности. Интрузии более молодого Имандровского комплекса с возрастом около 2.45 млрд лет расслоены от ортопироксенитов до феррогаббро. Важной их особенностью является комагматическая связь с вулканитами. Все интрузивные комплексы образованы из бонинитоподобного мантийного источника, обогащенного литофильными компонентами. Для пород этих двух разновозрастных комплексов характерны свои отличительные геохимические особенности. В породах Мончегорского и Федорово-Пан­ского комплексов наблюдается отчетливая зависимость накопления редкоземельных элементов (РЗЭ) от основности пород, нефракционированный «плоский» характер спектра РЗЭ и незначительно проявленные положительные Eu аномалии. В породах Имандровского комплекса уровень накопления РЗЭ сравнительно более высокий. Спектр РЗЭ в них отличается более фракционированным характером легких редкоземельных элементов (РЗЭ) при «плоском» распределении тяжелых редкоземельных элементов (РЗЭ) и отчетливо выраженными Eu аномалиями. Породы всех интрузивных комплексов характеризуются преимущественно отрицательными значениями параметра eNd(T), при этом в породах Мончегорского комплекса распределение значений eNd более гетерогенное, чем в породах Федорово-Панского комплекса. С интрузивными комплексами ИВС пространственно и генетически связаны месторождения и проявления Cr, комплексных платинометально (ЭПГ)-Cu-Ni и малосульфидных Pt-Pd руд мирового уровня. Стратиформное хромовое оруденение представлено Сопчеозерским месторождением (Мончеплутон Мончегорского комплекса) и месторождением Большая Варака (одноименная интрузия Имандровского комплекса). Комплексные ЭПГ-Cu-Ni месторождения – приурочены к Мончегорскому плутону. Они присутствуют в жильных рудах массивов Ниттис-Кумужья-Травяная (отработаны) и Сопчи, жильных ЭПГ – Cu, инъекционных существенно Ni рудах и донной залежи массива Ниттис-Кумужья-Травяная, а также в «критическом» горизонте Нюда. Малосульфидные Pt-Pd руды были выявлены в течение последних 10–15 лет и являются новыми для Кольского региона. Они делятся на два основных типа: стратиформные (рифовые), гармоничные с расслоенностью массивов, и базальные, локализованные в пределах нижних краевых зон. К первому типу относятся месторождения Киевей (Западно-Панский массив Федорово-Панского комплекса), 330-го горизонта Сопчи и Вурэчуайвенч (Мончеплутон Мончегорского комплекса), ко второму – Федоровотундровское (Федорово-Панский комплекс), Южносопчинское и Лойпишнюн (Мончетундровский массив Мончегорского комплекса). 

AGILE detection of delayed gamma-ray emission from GRB 080514B

GRB 080514B is the first gamma ray burst (GRB), since the time of EGRET, for which individual photons of energy above several tens of MeV have been detected with a pair-conversion tracker telescope. This burst was discovered with the Italian AGILE gamma-ray satellite. The GRB was localized with a cooperation by AGILE and the interplanetary network (IPN). The gamma-ray imager (GRID) estimate of the position, obtained before the SuperAGILE-IPN localization, is found to be consistent with the burst position. The hard X-ray emission observed by SuperAGILE lasted about 7 s, while there is evidence that the emission above 30 MeV extends for a longer duration (at least ~13 s). Similar behavior was seen in the past from a few other GRBs observed with EGRET. However, the latter measurements were affected, during the brightest phases, by instrumental dead time effects, resulting in only lower limits to the burst intensity. Thanks to the small dead time of the AGILE/GRID we could assess that in the case of GRB 080514B the gamma-ray to X-ray flux ratio changes significantly between the prompt and extended emission phase.Comment: A&A letters, in pres

Gauge Boson - Gauge Boson Scattering in Theories with Large Extra Dimensions

We consider the scattering amplitudes of the form V_1 V_2 -> V_3 V_4, where V_i=\gamma, Z, W or g(=gluon) are the Standard Model gauge bosons, due to graviton exchange in Kaluza-Klein theories with large extra dimensions. This leads to a number of experimentally viable signatures at high energy leptonic and hadronic colliders. We discuss the observability or future limits on the scale of the gravitational interactions (m_D), that may be obtained at an e+e- Next Linear Collider (NLC) and at the LHC, by studying some of these type of gauge boson scattering processes. We find that the attainable limits through these type of processes are: m_D > 3 TeV at the NLC and m_D > 6 TeV at the LHC.Comment: 27 pages, plain latex, 7 figures embadded in the text using epsfi

Low energy polarization sensitivity of the Gas Pixel Detector

An X-ray photoelectric polarimeter based on the Gas Pixel Detector has been proposed to be included in many upcoming space missions to fill the gap of about 30 years from the first (and to date only) positive measurement of polarized X-ray emission from an astrophysical source. The estimated sensitivity of the current prototype peaks at an energy of about 3 keV, but the lack of readily available polarized sources in this energy range has prevented the measurement of detector polarimetric performances. In this paper we present the measurement of the Gas Pixel Detector polarimetric sensitivity at energies of a few keV and the new, light, compact and transportable polarized source that was devised and built to this aim. Polarized photons are produced, from unpolarized radiation generated with an X-ray tube, by means of Bragg diffraction at nearly 45 degrees. The employment of mosaic graphite and flat aluminum crystals allow the production of nearly completely polarized photons at 2.6, 3.7 and 5.2 keV from the diffraction of unpolarized continuum or line emission. The measured modulation factor of the Gas Pixel Detector at these energies is in good agreement with the estimates derived from a Monte Carlo software, which was up to now employed for driving the development of the instrument and for estimating its low energy sensitivity. In this paper we present the excellent polarimetric performance of the Gas Pixel Detector at energies where the peak sensitivity is expected. These measurements not only support our previous claims of high sensitivity but confirm the feasibility of astrophysical X-ray photoelectric polarimetry.Comment: 15 pages, 12 figures. Accepted for publication in NIM

Electrodynamics of Magnetars: Implications for the Persistent X-ray Emission and Spindown of the Soft Gamma Repeaters and Anomalous X-ray Pulsars

(ABBREVIATED) We consider the structure of neutron star magnetospheres threaded by large-scale electrical currents, and the effect of resonant Compton scattering by the charge carriers (both electrons and ions) on the emergent X-ray spectra and pulse profiles. In the magnetar model for the SGRs and AXPs, these currents are maintained by magnetic stresses acting deep inside the star. We construct self-similar, force-free equilibria of the current-carrying magnetosphere with a power-law dependence of magnetic field on radius, B ~ r^(-2-p), and show that a large-scale twist softens the radial dependence to p < 1. The spindown torque acting on the star is thereby increased in comparison with a vacuum dipole. We comment on the strength of the surface magnetic field in the SGR and AXP sources, and the implications of this model for the narrow measured distribution of spin periods. A magnetosphere with a strong twist, B_\phi/B_\theta = O(1) at the equator, has an optical depth ~ 1 to resonant cyclotron scattering, independent of frequency (radius), surface magnetic field strength, or charge/mass ratio of the scattering charge. When electrons and ions supply the current, the stellar surface is also heated by the impacting charges at a rate comparable to the observed X-ray output of the SGR and AXP sources, if B_{dipole} ~ 10^{14} G. Redistribution of the emerging X-ray flux at the ion and electron cyclotron resonances will significantly modify the emerging pulse profile and, through the Doppler effect, generate a non-thermal tail to the X-ray spectrum. The sudden change in the pulse profile of SGR 1900+14 after the 27 August 1998 giant flare is related to an enhanced optical depth to electron cyclotron scattering, resulting from a sudden twist imparted to the external magnetic field.Comment: 31 January 2002, minor revisions, new section 5.4.