{"results":[{"id":"crossref_10.21070/ups.8652","title":"E-Comic Astro Kids Explore Milky Way","authors":[{"name":"Febi Talitha Salsabila"},{"name":"Machful Indrakurniawan"}],"abstract":"","source":"CrossRef","year":2025,"language":"en","subjects":null,"doi":"10.21070/ups.8652","url":"https://doi.org/10.21070/ups.8652","is_open_access":true,"published_at":"","score":69},{"id":"arxiv_2408.07474","title":"Debiasing astro-Photometric Observations with Corrections Using Statistics (DePhOCUS)","authors":[{"name":"Tobias Hoffmann"},{"name":"Marco Micheli"},{"name":"Juan Luis Cano"},{"name":"Maxime Devogèle"},{"name":"Davide Farnocchia"},{"name":"Petr Pravec"},{"name":"Peter Vereš"},{"name":"Björn Poppe"}],"abstract":"Photometric measurements allow the determination of an asteroid's absolute magnitude, which often represents the sole means to infer its size. Photometric observations can be obtained in a variety of filters that can be unique to a specific observatory. Those observations are then calibrated into specific bands with respect to reference star catalogs. In order to combine all the different measurements for evaluation, photometric observations need to be converted to a common band, typically V-band. Current band-correction schemes in use by IAU's Minor Planet Center, JPL's Center for Near Earth Object Studies and ESA's NEO Coordination Centre use average correction values for the apparent magnitude derived from photometry of asteroids as the corrections are dependent on the typically unknown spectrum of the object to be corrected. By statistically analyzing the photometric residuals of asteroids, we develop a new photometric correction scheme that does not only consider the band, but also accounts for reference catalog and observatory. We describe a new statistical photometry correction scheme for asteroid observations with debiased corrections. Testing this scheme on a reference group of asteroids, we see a 36% reduction in the photometric residuals. Moreover, the new scheme leads to a more accurate and debiased determination of the H-G magnitude system and, in turn, to more reliable inferred sizes. We discuss the significant shift in the corrections with this \"DePhOCUS\" debiasing system, its limitations, and the impact for photometric and physical properties of all asteroids, especially Near-Earth Objects.","source":"arXiv","year":2024,"language":"en","subjects":["astro-ph.EP","astro-ph.IM"],"doi":"10.1016/j.icarus.2024.116366","url":"https://arxiv.org/abs/2408.07474","pdf_url":"https://arxiv.org/pdf/2408.07474","is_open_access":true,"published_at":"2024-08-14T11:34:48Z","score":68},{"id":"arxiv_2305.11111","title":"PPDONet: Deep Operator Networks for Fast Prediction of Steady-State Solutions in Disk-Planet Systems","authors":[{"name":"Shunyuan Mao"},{"name":"Ruobing Dong"},{"name":"Lu Lu"},{"name":"Kwang Moo Yi"},{"name":"Sifan Wang"},{"name":"Paris Perdikaris"}],"abstract":"We develop a tool, which we name Protoplanetary Disk Operator Network (PPDONet), that can predict the solution of disk-planet interactions in protoplanetary disks in real-time. We base our tool on Deep Operator Networks (DeepONets), a class of neural networks capable of learning non-linear operators to represent deterministic and stochastic differential equations. With PPDONet we map three scalar parameters in a disk-planet system -- the Shakura \\\u0026 Sunyaev viscosity $α$, the disk aspect ratio $h_\\mathrm{0}$, and the planet-star mass ratio $q$ -- to steady-state solutions of the disk surface density, radial velocity, and azimuthal velocity. We demonstrate the accuracy of the PPDONet solutions using a comprehensive set of tests. Our tool is able to predict the outcome of disk-planet interaction for one system in less than a second on a laptop. A public implementation of PPDONet is available at \\url{https://github.com/smao-astro/PPDONet}.","source":"arXiv","year":2023,"language":"en","subjects":["astro-ph.EP","astro-ph.IM","cs.LG"],"doi":"10.3847/2041-8213/acd77f","url":"https://arxiv.org/abs/2305.11111","pdf_url":"https://arxiv.org/pdf/2305.11111","is_open_access":true,"published_at":"2023-05-18T16:53:35Z","score":67},{"id":"arxiv_2205.08212","title":"The specific heat of astro-materials: Review of theoretical concepts, materials and techniques","authors":[{"name":"Jens Biele"},{"name":"Matthias Grott"},{"name":"Michael E. Zolensky"},{"name":"Artur Benisek"},{"name":"Edgar Dachs"}],"abstract":"We provide detailed background, theoretical and practical, on the specific heat cp of minerals and mixtures thereof, 'astro-materials', as well as background information on common minerals and other relevant solid substances found on the surfaces of solar system bodies. Furthermore, we demonstrate how to use specific heat and composition data for lunar samples and meteorites as well as a new database of endmember mineral heat capacities (the result of an extensive literature review) to construct reference models for the isobaric specific heat cP as a function of temperature for common solar system materials. Using a (generally linear) mixing model for the specific heat of minerals allows extrapolation of the available data to very low and very high temperatures, such that models cover the temperature range between 10 and 1000 K at least (and pressures from zero up to several kbars). We describe a procedure to estimate cp(T) for virtually any solid solar system material with a known mineral composition, e.g., model specific heat as a function of temperature for a number of typical meteorite classes with known mineralogical compositions. We present, as examples, the cp(T) curves of a number of well-described laboratory regolith analogues, as well as for planetary ices and 'tholins' in the outer solar system. Part II will review and present the heat capacity database for minerals and compounds and part III is going to cover applications, standard reference compositions, cp(T) curves and a comparison with new and literature experimental data.","source":"arXiv","year":2022,"language":"en","subjects":["astro-ph.EP","cond-mat.mtrl-sci","physics.class-ph","physics.geo-ph"],"doi":"10.1007/s10765-022-03046-5","url":"https://arxiv.org/abs/2205.08212","pdf_url":"https://arxiv.org/pdf/2205.08212","is_open_access":true,"published_at":"2022-05-17T10:16:25Z","score":66},{"id":"arxiv_2007.07828","title":"ExoTiC-ISM: A Python package for marginalised exoplanet transit parameters across a grid of systematic instrument models","authors":[{"name":"Iva Laginja"},{"name":"Hannah R. Wakeford"}],"abstract":"To address the the problem of calibration of instrument systematics in transit light curves, we present the Python package ExoTiC-ISM. Transit spectroscopy can reveal many different chemical components in exoplanet atmospheres, but such results depend on well-calibrated transit light curve observations. Each transit data set will contain instrument systematics that depend on the instrument used and will need to be calibrated out with an instrument systematic model. The proposed solution in Wakeford et al. (2016) (arXiv:1601.02587 [astro-ph.EP]) is to use a marginalisation across a grid of systematic models in order to retrieve marginalised transit parameters. Doing this over observations in multiple wavelengths yields a robust transmission spectrum of an exoplanet. ExoTiC-ISM provides tools to perform this analysis, and its current capability contains a systematic grid that is applicable to the Wide Field Camera 3 (WFC3) detector on the Hubble Space Telescope (HST), particularly for the two infrared grisms G141 and G102. By modularisation of the code and implementation of more systematic grids, ExoTiC-ISM can be used for other instruments, and an implementation for select detectors on the James Webb Space Telescope (JWST) will provide robust transit spectra in the future.","source":"arXiv","year":2020,"language":"en","subjects":["astro-ph.IM","astro-ph.EP"],"doi":"10.21105/joss.02281","url":"https://arxiv.org/abs/2007.07828","pdf_url":"https://arxiv.org/pdf/2007.07828","is_open_access":true,"published_at":"2020-07-15T16:51:22Z","score":64},{"id":"arxiv_2003.13052","title":"The CARMENES search for exoplanets around M dwarfs. A super-Earth planet orbiting HD 79211 (GJ 338 B)","authors":[{"name":"E. González-Álvarez"},{"name":"M. R. Zapatero Osorio"},{"name":"J. A. Caballero"},{"name":"J. Sanz-Forcada"},{"name":"V. J. S. Béjar"},{"name":"L. González-Cuesta"},{"name":"S. Dreizler"},{"name":"F. F. Bauer"},{"name":"E. Rodríguez"},{"name":"L. Tal-Or"},{"name":"M. Zechmeister"},{"name":"D. Montes"},{"name":"M. J. López-González"},{"name":"I. Ribas"},{"name":"A. Reiners"},{"name":"A. Quirrenbach"},{"name":"P. J. Amado"},{"name":"G. Anglada-Escudé"},{"name":"M. Azzaro"},{"name":"M. Cortés-Contreras"},{"name":"A. P. Hatzes"},{"name":"T. Henning"},{"name":"S. V. Jeffers"},{"name":"A. Kaminski"},{"name":"M. Kürster"},{"name":"M. Lafarga"},{"name":"J. C. Morales"},{"name":"E. Pallé"},{"name":"M. Perger"},{"name":"J. H. M. M. Schmitt"}],"abstract":"We report on radial velocity time series for two M0.0V stars, GJ338B and GJ338A, using the CARMENES spectrograph, complemented by ground-telescope photometry from Las Cumbres and Sierra Nevada observatories. We aim to explore the presence of small planets in tight orbits using the spectroscopic radial velocity technique. We obtained 159 and 70 radial velocity measurements of GJ338B and A, respectively, with the CARMENES visible channel. We also compiled additional relative radial velocity measurements from the literature and a collection of astrometric data that cover 200 a of observations to solve for the binary orbit. We found dynamical masses of 0.64$\\pm$0.07M$_\\odot$ for GJ338B and 0.69$\\pm$0.07M$_\\odot$ for GJ338A. The CARMENES radial velocity periodograms show significant peaks at 16.61$\\pm$0.04 d (GJ338B) and 16.3$^{+3.5}_{-1.3}$ d (GJ338A), which have counterparts at the same frequencies in CARMENES activity indicators and photometric light curves. We attribute these to stellar rotation. GJ338B shows two additional, significant signals at 8.27$\\pm$0.01 and 24.45$\\pm$0.02 d, with no obvious counterparts in the stellar activity indices. The former is likely the first harmonic of the star's rotation, while we ascribe the latter to the existence of a super-Earth planet with a minimum mass of 10.27$^{+1.47}_{-1.38}$$M_{\\oplus}$ orbiting GJ338B. GJ338B b lies inside the inner boundary of the habitable zone around its parent star. It is one of the least massive planets ever found around any member of stellar binaries. The masses, spectral types, brightnesses, and even the rotational periods are very similar for both stars, which are likely coeval and formed from the same molecular cloud, yet they differ in the architecture of their planetary systems.","source":"arXiv","year":2020,"language":"en","subjects":["astro-ph.EP","astro-ph.SR"],"doi":"10.1051/0004-6361/201937050","url":"https://arxiv.org/abs/2003.13052","pdf_url":"https://arxiv.org/pdf/2003.13052","is_open_access":true,"published_at":"2020-03-29T15:16:44Z","score":64},{"id":"arxiv_2003.09659","title":"Narrowband large amplitude whistler-mode waves in the solar wind and their association with electrons: STEREO waveform capture observations","authors":[{"name":"C. A. Cattell"},{"name":"B. Short"},{"name":"A. W. Breneman"},{"name":"P. Grul"}],"abstract":"Large amplitude whistler waves at frequencies of 0.2 to 0.4 times electron cyclotron frequency are frequently observed in the solar wind. The waves are obliquely propagating close to the resonance cone, with significant electric fields parallel to the background magnetic field, enabling strong interactions with electrons. Propagation angles are distinctly different from whistlers usually observed in the solar wind, and amplitudes are significantly larger. Waves occur most often in association with stream interaction regions (SIRs), and are often close-packed. 68 percent of the 54 SIRs had narrowband whistler groups; 33 percent of the nine interplanetary coronal mass ejections had coherent groups. Although wave occurrence as a function of the electron temperature anisotropy and parallel beta is constrained by the thresholds for the whistler temperature anisotropy and firehose instabilities, neither is consistent with observed wave properties. We show for the first time that comparisons of wave data to thresholds for the electron beam driven instability (beam speed greater than twice the electron Alfven speed) and to the whistler heat flux fan instability indicate that either might destabilize the narrowband waves. In contrast, the less coherent waves, on average, are associated with zero or near zero heat flux and much higher electron Alfven speeds, without higher energy beams. This suggests that the less coherent waves may be more effective in regulating the electron heat flux, or that the scattering and energization of solar wind electrons by the narrowband waves results in broadening of the waves. The highly oblique propagation and large amplitudes of both the narrowband and less coherent whistlers enable resonant interactions with electrons over a broad energy range, and, unlike parallel whistlers does not require that the electrons and waves counter-propagate.","source":"arXiv","year":2020,"language":"en","subjects":["physics.space-ph","astro-ph.EP","astro-ph.SR"],"doi":"10.3847/1538-4357/ab961f","url":"https://arxiv.org/abs/2003.09659","pdf_url":"https://arxiv.org/pdf/2003.09659","is_open_access":true,"published_at":"2020-03-21T13:33:33Z","score":64},{"id":"arxiv_2002.07938","title":"A slow-down time-transformed symplectic integrator for solving the few-body problem","authors":[{"name":"Long Wang"},{"name":"Keigo Nitadori"},{"name":"Junichiro Makino"}],"abstract":"An accurate and efficient method dealing with the few-body dynamics is important for simulating collisional N-body systems like star clusters and to follow the formation and evolution of compact binaries. We describe such a method which combines the time-transformed explicit symplectic integrator (Preto \u0026 Tremaine 1999; Mikkola \u0026 Tanikawa 1999) and the slow-down method (Mikkola \u0026 Aarseth 1996). The former conserves the Hamiltonian and the angular momentum for a long-term evolution, while the latter significantly reduces the computational cost for a weakly perturbed binary. In this work, the Hamilton equations of this algorithm are analyzed in detail. We mathematically and numerically show that it can correctly reproduce the secular evolution like the orbit averaged method and also well conserve the angular momentum. For a weakly perturbed binary, the method is possible to provide a few order of magnitude faster performance than the classical algorithm. A publicly available code written in the c++ language, SDAR, is available on GitHub (https://github.com/lwang-astro/SDAR). It can be used either as a stand alone tool or a library to be plugged in other $N$-body codes. The high precision of the floating point to 62 digits is also supported.","source":"arXiv","year":2020,"language":"en","subjects":["astro-ph.EP","astro-ph.IM","astro-ph.SR"],"doi":"10.1093/mnras/staa480","url":"https://arxiv.org/abs/2002.07938","pdf_url":"https://arxiv.org/pdf/2002.07938","is_open_access":true,"published_at":"2020-02-19T00:24:21Z","score":64},{"id":"arxiv_2006.13324","title":"Analysis of HAT-P-23 b, Qatar-1 b, WASP-2 b, and WASP-33 b with an Optimized EXOplanet Transit Interpretation Code","authors":[{"name":"Sujay Nair"},{"name":"Jonathan Varghese"},{"name":"Kalée Tock"}],"abstract":"The ability for citizen scientists to analyze image data and search for exoplanets using images from small telescopes has the potential to greatly accelerate the search for exoplanets. Recent work on the Exoplanet Transit Interpretation Code (EXOTIC) enables the generation of high-quality light curves of exoplanet transits given such image data. However, on large image datasets, the photometric analysis of the data and fitting light curves can be a time-consuming process. In this work, we first optimize portions of the EXOTIC codebase to enable faster image processing and curve fitting. Specifically, we limited repetitive computation on fitting centroids with various apertures and annuli. Moreover, this speedup is scaled linearly based on the number of FITS files. After testing on existing HAT-P-32 b data and newer HAT-P-23 b data, our best demonstration was approximately a 5x speedup, though that factor increases given a larger number of FITS files. Utilizing the accelerated code, we analyzed transits of HAT-P-23 b, Qatar-1 b, WASP-2 b, and WASP-33 b using data captured by the 16\" SRO telescope operated by Boyce-Astro.","source":"arXiv","year":2020,"language":"en","subjects":["astro-ph.EP","astro-ph.IM"],"url":"https://arxiv.org/abs/2006.13324","pdf_url":"https://arxiv.org/pdf/2006.13324","is_open_access":true,"published_at":"2020-06-23T20:46:48Z","score":64},{"id":"arxiv_1904.12790","title":"Astro 2020: Astromineralogy of interstellar dust with X-ray spectroscopy","authors":[{"name":"Lia Corrales"},{"name":"Lynne Valencic"},{"name":"Elisa Costantini"},{"name":"Javier Garcia"},{"name":"Efrain Gatuzz"},{"name":"Tim Kallman"},{"name":"Julia Lee"},{"name":"Norbert Schulz"},{"name":"Sascha Zeegers"},{"name":"Claude Canizares"},{"name":"Bruce Draine"},{"name":"Sebastian Heinz"},{"name":"Edmund Hodges-Kluck"},{"name":"Edward B. Jenkins"},{"name":"Frits Paerels"},{"name":"Randall K. Smith"},{"name":"Tea Temim"},{"name":"Joern Wilms"},{"name":"Daniel W. Savin"}],"abstract":"X-ray absorption fine structure (XAFS) in the 0.2-2 keV band is a crucial component in multi-wavelength studies of dust mineralogy, size, and shape -- parameters that are necessary for interpreting astronomical observations and building physical models across all fields, from cosmology to exoplanets. Despite its importance, many fundamental questions about dust remain open. What is the origin of the dust that suffuses the interstellar medium (ISM)? Where is the missing interstellar oxygen? How does iron, predominantly produced by Type Ia supernovae, become incorporated into dust? What is the main form of carbon in the ISM, and how does it differ from carbon in stellar winds? The next generation of X-ray observatories, employing microcalorimeter technology and $R \\equiv λ/Δλ\\geq 3000$ gratings, will provide pivotal insights for these questions by measuring XAFS in absorption and scattering. However, lab measurements of mineralogical candidates for astrophysical dust, with R \u003e 1000, are needed to fully take advantage of the coming observations.","source":"arXiv","year":2019,"language":"en","subjects":["astro-ph.EP","astro-ph.HE"],"url":"https://arxiv.org/abs/1904.12790","pdf_url":"https://arxiv.org/pdf/1904.12790","is_open_access":true,"published_at":"2019-04-29T16:07:27Z","score":63},{"id":"arxiv_1910.00222","title":"The Role of NewSpace in Furthering Canadian Astronomy","authors":[{"name":"Aaron C. Boley"},{"name":"David Kendall"},{"name":"Michael Byers"},{"name":"Frederic J. Grandmont"},{"name":"Cameron Byers"},{"name":"Jennifer Busler"},{"name":"William MacDonald Evans"},{"name":"Brett Gladman"},{"name":"Tanya Harrison"},{"name":"Catherine Johnson"}],"abstract":"[Highly abridged, from executive summary] As much as NewSpace presents opportunities, there are significant challenges that must be overcome, requiring engagement with policy makers to influence domestic and international space governance. Failure to do so could result in a range of long-lasting negative outcomes for science and space stewardship. How will the Canadian astronomical community engage with NewSpace? What are the implications for NewSpace on the astro-environment, including Earth orbits, lunar and cis-lunar orbits, and surfaces of celestial bodies? This white paper analyzes the rapid changes in space use and what those changes could mean for Canadian astronomers. Our recommendations are as follows: Greater cooperation between the astronomical and the Space Situational Awareness communities is needed. Build closer ties between the astronomical community and Global Affairs Canada (GAC). Establish a committee for evaluating the astro-environmental impacts of human space use, including on and around the Moon and other bodies. CASCA and the Tri-Council should coordinate to identify programs that would enable Canadian astronomers to participate in pay-for-use services at appropriate funding levels. CASCA should continue to foster a relationship with CSA, but also build close ties to the private space industry. Canadian-led deep space missions are within Canada's capabilities, and should be pursued.","source":"arXiv","year":2019,"language":"en","subjects":["astro-ph.IM","astro-ph.EP"],"doi":"10.5281/zenodo.3755907","url":"https://arxiv.org/abs/1910.00222","pdf_url":"https://arxiv.org/pdf/1910.00222","is_open_access":true,"published_at":"2019-10-01T06:53:55Z","score":63},{"id":"arxiv_1912.01911","title":"Global Site Selection for Astronomy","authors":[{"name":"N. Aksaker"},{"name":"S. K. Yerli"},{"name":"M. A. Erdoğan"},{"name":"Z. Kurt"},{"name":"K. Kaba"},{"name":"M. Bayazit"},{"name":"C. Yesilyaprak"}],"abstract":"A global site selection for astronomy was performed with 1 km spatial resolution ($\\sim$ 1 Giga pixel in size) using long term and up-to-date datasets to classify the entire terrestrial surface on the Earth. Satellite instruments are used to get the following datasets of Geographical Information System (GIS) layers: Cloud Coverage, Digital Elevation Model, Artificial Light, Precipitable Water Vapor, Aerosol Optical Depth, Wind Speed and Land Use -- Land Cover. A Multi Criteria Decision Analysis (MCDA) technique is applied to these datasets creating four different series where each layer will have a specific weight. We introduce for the first time a ``Suitability Index for Astronomical Sites'' namely, SIAS. This index can be used to find suitable locations and to compare different sites or observatories. Mid-western Andes in South America and Tibetan Plateau in west China were found to be the best in all SIAS Series. Considering all the series, less than 3 \\% of all terrestrial surfaces are found to be the best regions to establish an astronomical observatory. In addition to this, only approximately 10 \\% of all current observatories are located in good locations in all SIAS series. Amateurs, institutions or countries aiming to construct an observatory could create a short-list of potential site locations using layout of SIAS values for each country without spending time and budget.The outcomes and datasets of this study has been made available through a web site, namely ``Astro GIS Database'' on \\texttt{\\url{www.astrogis.org}}.","source":"arXiv","year":2019,"language":"en","subjects":["astro-ph.IM","astro-ph.EP"],"doi":"10.1093/mnras/staa201","url":"https://arxiv.org/abs/1912.01911","pdf_url":"https://arxiv.org/pdf/1912.01911","is_open_access":true,"published_at":"2019-12-04T11:48:52Z","score":63},{"id":"crossref_10.1103/physrevd.97.061902","title":"Windings of twisted strings","authors":[{"name":"Eduardo Casali"},{"name":"Piotr Tourkine"}],"abstract":"","source":"CrossRef","year":2018,"language":"en","subjects":null,"doi":"10.1103/physrevd.97.061902","url":"https://doi.org/10.1103/physrevd.97.061902","is_open_access":true,"citations":12,"published_at":"","score":62.36},{"id":"arxiv_1810.05529","title":"Statistical Modeling of an astro-comb for high precision radial velocity observation","authors":[{"name":"Zhao Fei"},{"name":"Zhao Gang"},{"name":"Liu Yujuan"},{"name":"Wang Liang"},{"name":"Wang Huijuan"},{"name":"Li Hongbin"},{"name":"Ye Huiqi"},{"name":"Hao Zhibo"},{"name":"Xiao Dong"},{"name":"Zhang Junbo"},{"name":"Kellermann Hanna"},{"name":"Grupp Frank"}],"abstract":"The advent of the laser frequency comb as the wavelength calibration unit allows us to measure the radial velocity at $cm\\ s^{-1}$ precision level with high stability in long-term, which enable the possibility of the detection of Earth-twins around solar-like stars. Recent study shows that the laser frequency comb can also be used to measure and study the precision of the instrumental system including the variations of line profile and the systematic uncertainty and instrumental drift. In this paper, we present the stringent analysis of a laser frequency comb(LFC) system with 25GHz repetition frequency on a R$\\sim$50,000 spectrograph with the wavelength spanning from 5085Å\\ to 7380Å. We report a novel fitting model optimized for the comb line profile, the constrained double Gaussian. The constraint condition is set as $\\left|μ_{1,2} - μ\\right| \u003c\\sqrt{2ln2}σ$. We introduce Bayesian information criterion to test various models. Compared to the traditional Gaussian model, the CDG(Constrained Double Gaussians) model provides much better goodness of fit. We apply the CDG model to the observed comb data to demonstrate the improvement of RV precision with CDG model. We find that the improvement of CDG model is about 40\\%$\\sim$60\\% for wavelength calibration precision. We also consider the application to use the LFC and CDG model as a tool to characterize the line shape variation across the detector. The motivation of this work is to measure and understand the details of the comb lines including their asymmetry and behaviors under various conditions, which plays a significant role in the simultaneous calibration process and cross-correlation function method to determine the Doppler shift at high precision level.","source":"arXiv","year":2018,"language":"en","subjects":["astro-ph.IM","astro-ph.EP"],"url":"https://arxiv.org/abs/1810.05529","pdf_url":"https://arxiv.org/pdf/1810.05529","is_open_access":true,"published_at":"2018-10-11T10:22:07Z","score":62},{"id":"arxiv_1702.02079","title":"Planetary Ring Dynamics -- The Streamline Formalism -- 2. Theory of Narrow Rings and Sharp Edges","authors":[{"name":"Pierre-Yves Longaretti"}],"abstract":"The present material covers the features of large scale ring dynamics in perturbed flows that were not addressed in part 1 (astro-ph/1606.00759); this includes an extensive coverage of all kinds of ring modes dynamics (except density waves which have been covered in part 1), the origin of ring eccentricities and mode amplitudes, and the issue of ring/gap confinement. This still leaves aside a number of important dynamical issues relating to the ring small scale structure, most notably the dynamics of self-gravitational wakes, of local viscous overstabilities and of ballistic transport processes.   As this material is designed to be self-contained, there is some 30% overlap with part 1. This work constitutes a preprint of Chapter 11 of the forthcoming Cambridge University book on rings (Planetary Ring Systems, Matt Tiscareno and Carl Murray, eds).","source":"arXiv","year":2017,"language":"en","subjects":["astro-ph.EP"],"url":"https://arxiv.org/abs/1702.02079","pdf_url":"https://arxiv.org/pdf/1702.02079","is_open_access":true,"published_at":"2017-02-07T16:15:29Z","score":61},{"id":"arxiv_1706.01907","title":"Is there anybody out there?","authors":[{"name":"Luis A. Anchordoqui"},{"name":"Susanna M. Weber"},{"name":"Jorge F. Soriano"}],"abstract":"The Fermi paradox is the discrepancy between the strong likelihood of alien intelligent life emerging (under a wide variety of assumptions) and the absence of any visible evidence for such emergence. We use this intriguing unlikeness to derive an upper limit on the fraction of living intelligent species that develop communication technology \u003cξ_{biotec}\u003e. \u003c...\u003e indicates average over all the multiple manners civilizations can arise, grow, and develop such technology, starting at any time since the formation of our Galaxy in any location inside it. Following Drake, we factorize \u003cξ_{biotec}\u003e as the product of the fractions in which: (i) life arises, (ii) intelligence develops, and (iii) communication technology is developed. In this approximation, the number of communicating intelligent civilizations that exist in the Galaxy at any given time is found to be N = \u003cζ_{astro}\u003e \u003cξ_{biotec}\u003e L_τ, where \u003cζ_{astro}\u003e is the average production rate of potentially habitable rocky planets with a long-lasting (~ 4 Gyr) ecoshell and L_τ is the length of time that a typical civilization communicates. We estimate the production rate of exoplanets in the habitable zone and using recent determinations of the rate of gamma-ray bursts (GRBs) and their luminosity function, we calculate the probability that a life-threatening (lethal) GRB could make a planet inhospitable to life, yielding \u003cζ_{astro}\u003e ~ 2 \\times 10^{-3} yr^-1. Our current measurement of N =0 then implies \u003cζ_{biotec}\u003e \u003c 5 \\times 10^{-3} at the 95\\% C.L., where we have taken L_τ\u003e 0.3 Myr such that c L_τ\u003e\u003e propagation distances of Galactic scales (~ 10 kpc), ensuring that any advanced civilization living in the Milky Way would be able to communicate with us.","source":"arXiv","year":2017,"language":"en","subjects":["astro-ph.HE","astro-ph.EP"],"url":"https://arxiv.org/abs/1706.01907","pdf_url":"https://arxiv.org/pdf/1706.01907","is_open_access":true,"published_at":"2017-06-06T18:11:22Z","score":61},{"id":"crossref_10.1016/s0167-8140(15)40325-1","title":"SP-0327: ASTRO accreditation programmes (APEx)-ASTRO","authors":[{"name":"P. Tripuraneni"}],"abstract":"","source":"CrossRef","year":2015,"language":"en","subjects":null,"doi":"10.1016/s0167-8140(15)40325-1","url":"https://doi.org/10.1016/s0167-8140(15)40325-1","is_open_access":true,"citations":1,"published_at":"","score":59.03},{"id":"crossref_10.1093/ofid/ofv133.1240","title":"Development of Anemia and Changes in Hemoglobin Concentrations With Amphotericin B Therapy for Cryptococcal Meningitis","authors":[{"name":"Lillian Tugume"},{"name":"COAT Trial and ASTRO-CM Trial Teams"},{"name":"Bozena Morawski"},{"name":"COAT Trial and ASTRO-CM Trial Teams"},{"name":"Mahsa Abassi"},{"name":"COAT Trial and ASTRO-CM Trial Teams"},{"name":"Nathan Bahr"},{"name":"COAT Trial and ASTRO-CM Trial Teams"},{"name":"Reuben Kiggundu"},{"name":"COAT Trial and ASTRO-CM Trial Teams"},{"name":"Henry Nabeta"},{"name":"COAT Trial and ASTRO-CM Trial Teams"},{"name":"Kathy Huppler Hullsiek"},{"name":"COAT Trial and ASTRO-CM Trial Teams"},{"name":"Taseera Kabanda"},{"name":"COAT Trial and ASTRO-CM Trial Teams"},{"name":"Abdu Musubire"},{"name":"COAT Trial and ASTRO-CM Trial Teams"},{"name":"Charlotte Schutz"},{"name":"COAT Trial and ASTRO-CM Trial Teams"},{"name":"Conrad Muzoora"},{"name":"COAT Trial and ASTRO-CM Trial Teams"},{"name":"Darlisha Williams"},{"name":"COAT Trial and ASTRO-CM Trial Teams"},{"name":"Melissa Rolfes"},{"name":"COAT Trial and ASTRO-CM Trial Teams"},{"name":"Graeme Meintjes"},{"name":"COAT Trial and ASTRO-CM Trial Teams"},{"name":"Joshua Rhein"},{"name":"COAT Trial and ASTRO-CM Trial Teams"},{"name":"David Meya"},{"name":"COAT Trial and ASTRO-CM Trial Teams"},{"name":"David Boulware"},{"name":"COAT Trial and ASTRO-CM Trial Teams"}],"abstract":"","source":"CrossRef","year":2015,"language":"en","subjects":null,"doi":"10.1093/ofid/ofv133.1240","url":"https://doi.org/10.1093/ofid/ofv133.1240","is_open_access":true,"published_at":"","score":59},{"id":"crossref_10.1093/ofid/ofv133.507","title":"Enhanced Consolidation Therapy With High-Dose Fluconazole and Sertraline Ameliorates Negative Outcomes Associated With Persistent Cerebrospinal Fluid Culture Positivity in Cryptococcal Meningitis","authors":[{"name":"Mahsa Abassi"},{"name":"on behalf of the ASTRO-CM Trial Team"},{"name":"Joshua Rhein"},{"name":"on behalf of the ASTRO-CM Trial Team"},{"name":"Bozena Morawski"},{"name":"on behalf of the ASTRO-CM Trial Team"},{"name":"Kathy H. Hullsiek"},{"name":"on behalf of the ASTRO-CM Trial Team"},{"name":"Lillian Tugume"},{"name":"on behalf of the ASTRO-CM Trial Team"},{"name":"Henry Nabeta"},{"name":"on behalf of the ASTRO-CM Trial Team"},{"name":"Reuben Kiggundu"},{"name":"on behalf of the ASTRO-CM Trial Team"},{"name":"Andrew Akampurira"},{"name":"on behalf of the ASTRO-CM Trial Team"},{"name":"Darlisha Williams"},{"name":"on behalf of the ASTRO-CM Trial Team"},{"name":"David Meya"},{"name":"on behalf of the ASTRO-CM Trial Team"},{"name":"David Boulware"},{"name":"on behalf of the ASTRO-CM Trial Team"}],"abstract":"","source":"CrossRef","year":2015,"language":"en","subjects":null,"doi":"10.1093/ofid/ofv133.507","url":"https://doi.org/10.1093/ofid/ofv133.507","is_open_access":true,"published_at":"","score":59},{"id":"crossref_10.1016/s0167-8140(15)41682-2","title":"EP-1690: Analysis of logbook in an educational institution and comparison with ASTRO, ESTRO and CNRM requirements","authors":[{"name":"L.G. Sapienza"},{"name":"M.L. Sucharski Figueiredo"},{"name":"M.J. Chen"},{"name":"A.C.A. Pellizzon"}],"abstract":"","source":"CrossRef","year":2015,"language":"en","subjects":null,"doi":"10.1016/s0167-8140(15)41682-2","url":"https://doi.org/10.1016/s0167-8140(15)41682-2","is_open_access":true,"published_at":"","score":59}],"total":378667,"page":1,"page_size":20,"sources":["CrossRef","arXiv"],"query":"astro-ph.EP"}