cometadata/datacite-rtg-text-other-reclassification-records huggingface dataset:
Numerical Star-Formation Studies -- A Status Report
Creators: name: Klessen, Ralf S.
name: Krumholz, Mark R.
name: Heitsch, Fabian
Publisher: name: arXiv
Year: 2009
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: Instrumentation and Methods for Astrophysics (astro-ph.IM)
subject: FOS: Physical sciences

description: The formation of stars is a key process in astrophysics. Detailed knowledge of the physical mechanisms that govern stellar birth is a prerequisite for understanding the formation and evolution of our galactic home, the Milky Way. A theory of star formation is an essential part of any model for the origin of our solar system and of planets around other stars. Despite this pivotal importance, and despite many decades of research, our understanding of the processes that initiate and regulate star formation is still limited. Stars are born in cold interstellar clouds of molecular hydrogen gas. Star formation in these clouds is governed by the complex interplay between the gravitational attraction in the gas and agents such as turbulence, magnetic fields, radiation and thermal pressure that resist compression. The competition between these processes determines both the locations at which young stars form and how much mass they ultimately accrete. It plays out over many orders of magnitude in space and time, ranging from galactic to stellar scales. In addition, star formation is a highly stochastic process in which rare and hard-to-predict events, such as the formation of very massive stars and the resulting feedback, can play a dominant role in determining the evolution of a star-forming cloud. As a consequence of the wide range of scales and processes that control star formation, analytic models are usually restricted to highly idealized cases. These can yield insight, but the complexity of the problem means that they must be used in concert with large-scale numerical simulations. Here we summarize the state of modern star formation theory and review the recent advances in numerical simulation techniques.
description: Invited Review to appear on Advanced Science Letters (ASL), Special Issue on Computational Astrophysics, edited by Lucio Mayer (32 pages, 10 figures)
Timing analysis of Swift J0243.6+6124 with NICER and Fermi/GBM during the decay phase of the 2017-2018 outburst
Creators: name: Serim, M. M.
name: Dönmez, Ç. K.
name: Serim, D.
name: Ducci, L.
name: Baykal, A.
name: Santangelo, A.
Publisher: name: arXiv
Year: 2023
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: We present a timing and noise analysis of the Be/X-ray binary system Swift J0243.6+6124 during its 2017-2018 super-Eddington outburst using NICER/XTI observations. We apply a synthetic pulse timing analysis to enrich the Fermi/GBM spin frequency history of the source with the new measurements from NICER/XTI. We show that the pulse profiles switch from double-peaked to single-peaked when the X-ray luminosity drops below $\sim$$7\times 10^{36}$ erg s$^{-1}$. We suggest that this transitional luminosity is associated with the transition from a pencil beam pattern to a hybrid beam pattern when the Coulomb interactions become ineffective to decelerate the accretion flow, which implies a dipolar magnetic field strength of $\sim$$5\times 10^{12}$ G. We also obtained the power density spectra (PDS) of the spin frequency derivative fluctuations. The red noise component of the PDS is found to be steeper ($ω^{-3.36}$) than the other transient accreting sources. We find significantly high noise strength estimates above the super-Eddington luminosity levels, which may arise from the torque fluctuations due to interactions with the quadrupole fields at such levels.
description: 18 pages, 6 figures. Accepted for publication in MNRAS
Teacher training toolkit supporting the implementation and the dissemination of the MOBAK App
Creators: name: Lüthy, Pascale
name: Schole, Lucas
name: Adamakis, Manolis
name: Bund, Andreas
name: Ennigkeit, Fabienne
name: Ferrari, Ilaria
name: Gerlach, Erin
name: Heim, Christopher
name: Masaryková, Dana
name: Mombarg, Remo
name: Niederkofler, Benjamin
name: Nolles, Janco
name: Vlček, Petr
name: Herrmann, Christian
Publisher: name: Pädagogische Hochschule Zürich
Year: 2024
Subjects: Mobak App
Basic motor skills
teacher training
guidance material for the implementation of the MOBAK App
diagnose and promote basic motor skills

description: excerpt from the publication

«The aim of the MOBAK App is to support teachers in the diagnosis and promotion of basic motor competencies. After participating in the teacher training, every teacher will be able to use the MOBAK app…1. … in physical education (PE) lessons to diagnose basic motor competencies.2. … to plan PE lessons to promote basic motor competencies.The teacher training is intended for all teachers who would like to familiarise themselves with the MOBAK concept and are interested in an app for diagnosing and promoting basic motor competencies. Teachers can use the material to offer further teacher trainings themselves.» [5]

→ Dutch Version: 10.5281/zenodo.10691870→ German Version: 10.5281/zenodo.10691980 → Slovak Version:  10.5281/zenodo.10691994

 

Further documents on the MOBAK APP:

Handbook and guidance material for the implementation of the MOBAK App → 10.5281/zenodo.10691652

Theoretical and methodological framework for the MOBAK App. Pedagogical strategy for the use of the MOBAK App in school physical education. → 10.5281/zenodo.10691463 

 Method and tool to evaluate the pilot implementation of the MOBAK App → 10.5281/zenodo.10684702

Pilot implementation and evaluation study report → 10.5281/zenodo.10843490 

 

Link to the App: Mobak - App on Google Play

Suggested citation for the app:

Lüthy, P., Schole, L., Ennigkeit, F., Ferrari, I., Niederkofler, B., Gerlach, E., Adamakis, M., Bund, A., Heck, S., Heim, C., Masaryková, D., Mombarg, R., Nolles, J., Scheuer, C., Vlček, P., Vrbas, J. & Herrmann, C. 2023. MOBAK App
description: +repphzhbib2023A
title: Ð­ÐºÑÐ¿ÐµÑÐ¸Ð¼ÐµÐ½ÑÐ°Ð»ÑÐ½ÑÐµ Ð¼ÐµÑÐ¾Ð´Ñ Ð¸ÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð¸Ð¹. ÐÑÐ½Ð¾Ð²Ñ Ð¼Ð°ÑÑ-ÑÐ¿ÐµÐºÑÑÐ¾Ð¼ÐµÑÑÐ¸Ð¸
title: ÑÑÐµÐ±Ð½Ð¾Ðµ Ð¿Ð¾ÑÐ¾Ð±Ð¸Ðµ
titleType: Subtitle
Creators: name: Ð¦ÑÐ±Ð¸Ð½, ÐÐ»ÐµÐ³
name: Ð¦ÑÐ±Ð¸Ð½, Ð®ÑÐ¸Ð¹
Publisher: name: ÐÐ·Ð´-Ð²Ð¾ ÐÐ¾Ð»Ð¸ÑÐµÑÐ½. ÑÐ½-ÑÐ°
Year: 2008
Subjects: ÐÐ°ÑÑ-ÑÐ¿ÐµÐºÑÑÐ¾Ð¼ÐµÑÑÐ¸Ñ

description: ÐÐ¾ÑÐ¾Ð±Ð¸Ðµ ÑÐ¾Ð¾ÑÐ²ÐµÑÑÑÐ²ÑÐµÑ Ð³Ð¾ÑÑÐ´Ð°ÑÑÑÐ²ÐµÐ½Ð½Ð¾Ð¼Ñ Ð¾Ð±ÑÐ°Ð·Ð¾Ð²Ð°ÑÐµÐ»ÑÐ½Ð¾Ð¼Ñ ÑÑÐ°Ð½Ð´Ð°ÑÑÑ Ð´Ð¸ÑÑÐ¸Ð¿Ð»Ð¸Ð½Ñ ÐÐÐ.Ð¤.09 Ð½Ð°Ð¿ÑÐ°Ð²Ð»ÐµÐ½Ð¸Ñ Ð¿Ð¾Ð´Ð³Ð¾ÑÐ¾Ð²ÐºÐ¸ Ð±Ð°ÐºÐ°Ð»Ð°Ð²ÑÐ¾Ð² 140400 Â«Ð¢ÐµÑÐ½Ð¸ÑÐµÑÐºÐ°Ñ ÑÐ¸Ð·Ð¸ÐºÐ°Â», Ð° ÑÐ°ÐºÐ¶Ðµ Ð¿ÑÐ¾Ð³ÑÐ°Ð¼Ð¼Ð°Ð¼ Ð¼Ð°Ð³Ð¸ÑÑÐµÑÑÐºÐ¾Ð¹ Ð¿Ð¾Ð´Ð³Ð¾ÑÐ¾Ð²ÐºÐ¸ Â«Ð¤Ð¸Ð·Ð¸ÐºÐ° Ð¼ÐµÐ´Ð¸ÑÐ¸Ð½ÑÐºÐ¸Ñ ÑÐµÑÐ½Ð¾Ð»Ð¾Ð³Ð¸Ð¹Â» Ð¸ Â«ÐÐµÐ´Ð¸ÑÐ¸Ð½ÑÐºÐ°Ñ Ð¸ Ð±Ð¸Ð¾Ð¸Ð½Ð¶ÐµÐ½ÐµÑÐ½Ð°Ñ ÑÐ¸Ð·Ð¸ÐºÐ°Â». ÐÐ·Ð»Ð¾Ð¶ÐµÐ½Ñ Ð¼ÐµÑÐ¾Ð´Ñ Ð¸ ÑÐ¸Ð·Ð¸ÐºÐ¾-ÑÐµÑÐ½Ð¸ÑÐµÑÐºÐ¸Ðµ Ð¾ÑÐ½Ð¾Ð²Ñ ÑÐ¾Ð²ÑÐµÐ¼ÐµÐ½Ð½Ð¾Ð¹ Ð¼Ð°ÑÑ-ÑÐ¿ÐµÐºÑÑÐ¾Ð¼ÐµÑÑÐ¸Ð¸. ÐÑÐ¸Ð²ÐµÐ´ÐµÐ½Ð¾ Ð¾Ð¿Ð¸ÑÐ°Ð½Ð¸Ðµ Ð¿ÑÐ¸Ð½ÑÐ¸Ð¿Ð¾Ð² Ð¼Ð°ÑÑ-ÑÐ¿ÐµÐºÑÑÐ¾Ð¼ÐµÑÑÐ¸ÑÐµÑÐºÐ¸Ñ Ð¸Ð·Ð¼ÐµÑÐµÐ½Ð¸Ð¹, Ð¾ÑÐ½Ð¾Ð² Ð¼Ð°ÑÑ-ÑÐ¿ÐµÐºÑÑÐ¾Ð¼ÐµÑÑÐ¸ÑÐµÑÐºÐ¸Ñ ÑÐºÑÐ¿ÐµÑÐ¸Ð¼ÐµÐ½ÑÐ°Ð»ÑÐ½ÑÑ Ð¸ÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð¸Ð¹, ÐºÐ¾Ð½ÑÑÑÑÐºÑÐ¸Ð¹ Ð¼Ð°ÑÑ-ÑÐ¿ÐµÐºÑÑÐ¾Ð¼ÐµÑÑÐ¾Ð², ÑÑÑÑÐ¾Ð¹ÑÑÐ²Ð° Ð¸Ñ ÑÐ·Ð»Ð¾Ð² Ð¸ Ð¿ÑÐ¾Ð¸ÑÑÐ¾Ð´ÑÑÐ¸Ñ Ð² Ð½Ð¸Ñ Ð¿ÑÐ¾ÑÐµÑÑÐ¾Ð². Ð Ð°ÑÑÐ¼Ð¾ÑÑÐµÐ½Ñ ÑÐ¾Ð²ÑÐµÐ¼ÐµÐ½Ð½ÑÐµ Ð¼Ð°ÑÑ-Ð°Ð½Ð°Ð»Ð¸Ð·Ð°ÑÐ¾ÑÑ, ÑÐµÐ³Ð¸ÑÑÑÐ°ÑÐ¾ÑÑ, ÐºÐ¾Ð¼Ð¿ÑÑÑÐµÑÐ½ÑÐµ ÑÑÑÑÐ¾Ð¹ÑÑÐ²Ð° ÑÐ¿ÑÐ°Ð²Ð»ÐµÐ½Ð¸Ñ Ð¼Ð°ÑÑ-ÑÐ¿ÐµÐºÑÑÐ¾Ð¼ÐµÑÑÐ¾Ð¼, Ð¼ÐµÑÐ¾Ð´Ñ Ð¾Ð±ÑÐ°Ð±Ð¾ÑÐºÐ¸ Ð¸ Ð¸Ð½ÑÐµÑÐ¿ÑÐµÑÐ°ÑÐ¸Ð¸ Ð¿Ð¾Ð»ÑÑÐ°ÐµÐ¼Ð¾Ð¹ Ð¸Ð½ÑÐ¾ÑÐ¼Ð°ÑÐ¸Ð¸. ÐÑÐµÐ´Ð½Ð°Ð·Ð½Ð°ÑÐµÐ½Ð¾ Ð´Ð»Ñ ÑÑÑÐ´ÐµÐ½ÑÐ¾Ð² Ð²ÑÑÑÐ¸Ñ ÑÑÐµÐ±Ð½ÑÑ Ð·Ð°Ð²ÐµÐ´ÐµÐ½Ð¸Ð¹, Ð¾Ð±ÑÑÐ°ÑÑÐ¸ÑÑÑ Ð¿Ð¾ Ð½Ð°Ð¿ÑÐ°Ð²Ð»ÐµÐ½Ð¸Ñ Ð¿Ð¾Ð´Ð³Ð¾ÑÐ¾Ð²ÐºÐ¸ 140400 Â«Ð¢ÐµÑÐ½Ð¸ÑÐµÑÐºÐ°Ñ ÑÐ¸Ð·Ð¸ÐºÐ°Â». ÐÐ¾Ð¶ÐµÑ Ð±ÑÑÑ ÑÐ°ÐºÐ¶Ðµ Ð¸ÑÐ¿Ð¾Ð»ÑÐ·Ð¾Ð²Ð°Ð½Ð¾ ÑÑÑÐ´ÐµÐ½ÑÐ°Ð¼Ð¸ ÑÐ¸Ð·Ð¸ÑÐµÑÐºÐ¸Ñ, Ð±Ð¸Ð¾Ð»Ð¾Ð³Ð¸ÑÐµÑÐºÐ¸Ñ Ð¸ ÑÐ¸Ð¼Ð¸ÑÐµÑÐºÐ¸Ñ ÑÐ¿ÐµÑÐ¸Ð°Ð»ÑÐ½Ð¾ÑÑÐµÐ¹ Ð²ÑÑÑÐ¸Ñ ÑÑÐµÐ±Ð½ÑÑ Ð·Ð°Ð²ÐµÐ´ÐµÐ½Ð¸Ð¹, Ð°ÑÐ¿Ð¸ÑÐ°Ð½ÑÐ°Ð¼Ð¸, Ð½Ð°ÑÑÐ½ÑÐ¼Ð¸ Ð¸ Ð¸Ð½Ð¶ÐµÐ½ÐµÑÐ½Ð¾-ÑÐµÑÐ½Ð¸ÑÐµÑÐºÐ¸Ð¼Ð¸ ÑÐ°Ð±Ð¾ÑÐ½Ð¸ÐºÐ°Ð¼Ð¸, Ð° ÑÐ°ÐºÐ¶Ðµ Ð¿Ð¾Ð»ÑÐ·Ð¾Ð²Ð°ÑÐµÐ»ÑÐ¼Ð¸ Ð¼Ð°ÑÑ-ÑÐ¿ÐµÐºÑÑÐ¾Ð¼ÐµÑÑÐ¾Ð².
description: ÐÐµÑÐ°ÑÐ°ÐµÑÑÑ Ð¿Ð¾ ÑÐµÑÐµÐ½Ð¸Ñ ÑÐµÐ´Ð°ÐºÑÐ¸Ð¾Ð½Ð½Ð¾-Ð¸Ð·Ð´Ð°ÑÐµÐ»ÑÑÐºÐ¾Ð³Ð¾ ÑÐ¾Ð²ÐµÑÐ° Ð¡Ð°Ð½ÐºÑ-ÐÐµÑÐµÑÐ±ÑÑÐ³ÑÐºÐ¾Ð³Ð¾ Ð³Ð¾ÑÑÐ´Ð°ÑÑÑÐ²ÐµÐ½Ð½Ð¾Ð³Ð¾ Ð¿Ð¾Ð»Ð¸ÑÐµÑÐ½Ð¸ÑÐµÑÐºÐ¾Ð³Ð¾ ÑÐ½Ð¸Ð²ÐµÑÑÐ¸ÑÐµÑÐ°.
Interface Modes and Their Instabilities in Accretion Disc Boundary Layers
Creators: name: Tsang, David
name: Lai, Dong
Publisher: name: arXiv
Year: 2008
Subjects: subject: Astrophysics (astro-ph)
subject: FOS: Physical sciences

description: We study global non-axisymmetric oscillation modes trapped near the inner boundary of an accretion disc. Observations indicate that some of the quasi-periodic oscillations (QPOs) observed in the luminosities of accreting compact objects (neutron stars, black holes and white dwarfs) are produced in the inner-most regions of accretion discs or boundary layers. Two simple models are considered in this paper: The magnetosphere-disc model consists of a thin Keplerian disc in contact with a uniformly rotating magnetosphere with and low plasma density, while the star-disc model involves a Keplerian disc terminated at the stellar atomosphere with high density and small density scale height. We find that the interface modes at the magnetosphere-disc boundary are generally unstable due to Rayleigh-Taylor and/or Kelvin-Helmholtz instabilities. However, differential rotation of the disc tends to suppress Rayleigh-Taylor instability and a sufficiently high disc sound speed (or temperature) is needed to overcome this suppression and to attain net mode growth. On the other hand, Kelvin-Helmholtz instability may be active at low disc sound speeds. We also find that the interface modes trapped at the boundary between a thin disc and an unmagnetized star do not suffer Rayleigh-Taylor or Kelvin-Helmholtz instability, but can become unstable due to wave leakage to large disc radii and, for sufficiently steep disc density distributions, due to wave absorption at the corotation resonance in the disc. The non-axisymmetric interface modes studied in this paper may be relevant to the high-frequency QPOs observed in some X-ray binaries and in cataclysmic variables.
description: 14 pages, 9 figures, submitted to MNRAS
title: Ð­ÐºÑÐ¿ÐµÑÐ¸Ð¼ÐµÐ½ÑÐ°Ð»ÑÐ½Ð¾Ðµ Ð¸ÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð¸Ðµ Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ñ Ð¿Ð»Ð°Ð·Ð¼Ñ Ð² Ð´Ð¸Ð°Ð¿Ð°Ð·Ð¾Ð½Ðµ ÑÐ°ÑÑÐ¾Ñ Ð¸Ð¾Ð½Ð½Ð¾-ÑÐ¸ÐºÐ»Ð¾ÑÑÐ¾Ð½Ð½Ð¾Ð³Ð¾ ÑÐµÐ·Ð¾Ð½Ð°Ð½ÑÐ° Ð½Ð° ÑÐ¾ÐºÐ°Ð¼Ð°ÐºÐµ Ð¢Ð£ÐÐÐ-3Ð
title: Ð²ÑÐ¿ÑÑÐºÐ½Ð°Ñ ÐºÐ²Ð°Ð»Ð¸ÑÐ¸ÐºÐ°ÑÐ¸Ð¾Ð½Ð½Ð°Ñ ÑÐ°Ð±Ð¾ÑÐ° Ð¼Ð°Ð³Ð¸ÑÑÑÐ°
titleType: Subtitle
Creators: name: ÐÐ°Ð»Ð°ÑÐµÐ½ÐºÐ¾Ð², ÐÐ²Ð°Ð½
Publisher: name: Ð¡Ð°Ð½ÐºÑ-ÐÐµÑÐµÑÐ±ÑÑÐ³ÑÐºÐ¸Ð¹ Ð¿Ð¾Ð»Ð¸ÑÐµÑÐ½Ð¸ÑÐµÑÐºÐ¸Ð¹ ÑÐ½Ð¸Ð²ÐµÑÑÐ¸ÑÐµÑ ÐÐµÑÑÐ° ÐÐµÐ»Ð¸ÐºÐ¾Ð³Ð¾
Year: 2018
Subjects: ÐÐ»Ð°Ð·Ð¼Ð° (ÑÐ¸Ð·.)
ÐÐ°Ð³Ð½Ð¸ÑÐ½ÑÐµ Ð»Ð¾Ð²ÑÑÐºÐ¸ Ð´Ð»Ñ Ð¿Ð»Ð°Ð·Ð¼Ñ

description: Ð ÑÐ°Ð±Ð¾ÑÐµ ÑÐ°ÑÑÐ¼Ð°ÑÑÐ¸Ð²Ð°ÐµÑÑÑ ÑÑÑÐµÐºÑ ÑÐ¼Ð¸ÑÑÐ¸Ð¸ Ð¸Ð¾Ð½Ð½Ð¾-ÑÐ¸ÐºÐ»Ð¾ÑÑÐ¾Ð½Ð½Ð¾Ð³Ð¾ Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ñ (ICE), Ð²Ð¾Ð·Ð½Ð¸ÐºÐ°ÑÑÐ¸Ð¹ Ð½Ð° ÑÐ¾ÐºÐ°Ð¼Ð°ÐºÐµ Ð¢Ð£ÐÐÐ-3Ð, Ð¸ÑÑÐ»ÐµÐ´ÑÑÑÑÑ ÑÐµÐ¶Ð¸Ð¼Ñ, Ð² ÐºÐ¾ÑÐ¾ÑÑÑ ÑÐµÐ³Ð¸ÑÑÑÐ¸ÑÑÐµÑÑÑ Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ðµ. ÐÐ»Ñ Ð½Ð°Ð±Ð»ÑÐ´ÐµÐ½Ð¸Ñ Ð¸Ð¾Ð½Ð½Ð¾-ÑÐ¸ÐºÐ»Ð¾ÑÑÐ¾Ð½Ð½Ð¾Ð³Ð¾ Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ñ Ð²Ð½ÐµÐ´ÑÐµÐ½Ð° Ð¼Ð¾Ð´ÐµÑÐ½Ð¸Ð·Ð¸ÑÐ¾Ð²Ð°Ð½Ð½Ð°Ñ Ð¼Ð°Ð³Ð½Ð¸ÑÐ½Ð°Ñ Ð´Ð¸Ð°Ð³Ð½Ð¾ÑÑÐ¸ÐºÐ°, Ð¿Ð¾Ð·Ð²Ð¾Ð»ÑÑÑÐ°Ñ Ð½Ð°Ð±Ð»ÑÐ´Ð°ÑÑ Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ðµ Ð²Ð´Ð¾Ð»Ñ Ð¿Ð¾Ð»Ð½Ð¾Ð³Ð¾ Ð¿Ð¾Ð»Ð¾Ð¸Ð´Ð°Ð»ÑÐ½Ð¾Ð³Ð¾ Ð¾Ð±ÑÐ¾Ð´Ð° Ð² ÑÐ°ÑÑÐ¾ÑÐ½Ð¾Ð¼ Ð´Ð¸Ð°Ð¿Ð°Ð·Ð¾Ð½Ðµ Ð´Ð¾ 100 ÐÐÑ. ÐÐ¾Ð´ÐµÑÐ½Ð¸Ð·Ð°ÑÐ¸Ñ Ð´Ð¸Ð°Ð³Ð½Ð¾ÑÑÐ¸ÐºÐ¸ Ð´Ð°Ð»Ð° Ð²Ð¾Ð·Ð¼Ð¾Ð¶Ð½Ð¾ÑÑÑ Ð¸Ð·ÑÑÐ°ÑÑ Ð¿Ð¾Ð»Ð¾Ð¸Ð´Ð°Ð»ÑÐ½ÑÑ ÑÑÑÑÐºÑÑÑÑ ÑÐµÐ³Ð¸ÑÑÑÐ¸ÑÑÐµÐ¼Ð¾Ð³Ð¾ Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ñ, Ð° ÑÐ°ÐºÐ¶Ðµ Ð¸ÑÑÐ»ÐµÐ´Ð¾Ð²Ð°ÑÑ Ð·Ð°Ð²Ð¸ÑÐ¸Ð¼Ð¾ÑÑÑ Ð¿Ð°ÑÐ°Ð¼ÐµÑÑÐ¾Ð² Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ñ Ð¾Ñ Ð¿Ð°ÑÐ°Ð¼ÐµÑÑÐ¾Ð² Ð¿Ð»Ð°Ð·Ð¼Ñ. ÐÑÑÐ²Ð»ÐµÐ½ Ð¿Ð¾ÑÐ¾Ð³Ð¾Ð²ÑÐ¹ ÑÐ°ÑÐ°ÐºÑÐµÑ Ð·Ð°Ð²Ð¸ÑÐ¸Ð¼Ð¾ÑÑÐ¸ Ð¸Ð½ÑÐµÐ½ÑÐ¸Ð²Ð½Ð¾ÑÑÐ¸ NBI ICE Ð¾Ñ Ð¿Ð»Ð¾ÑÐ½Ð¾ÑÑÐ¸ Ð¿Ð»Ð°Ð·Ð¼Ñ. ÐÐµÐ»Ð¸ÑÐ¸Ð½Ð° Ð¿Ð¾ÑÐ¾Ð³Ð° Ð¿ÑÐ¾Ð¿Ð¾ÑÑÐ¸Ð¾Ð½Ð°Ð»ÑÐ½Ð° ÑÐ½ÐµÑÐ³Ð¸Ð¸ Ð¸Ð½Ð¶ÐµÐºÑÐ¸Ð¸. ÐÐ»Ñ ICE Ð²Ð¾Ð·Ð½Ð¸ÐºÐ°ÑÑÐµÐ¹ Ð² Ð¾Ð¼Ð¸ÑÐµÑÐºÐ¾Ð¼ ÑÐµÐ¶Ð¸Ð¼Ðµ ÐºÐ¾ÑÑÐµÐ»ÑÑÐ¸Ð¸ Ñ Ð¿Ð»Ð¾ÑÐ½Ð¾ÑÑÑÑ Ð¸ Ð¼Ð°Ð³Ð½Ð¸ÑÐ½ÑÐ¼ Ð¿Ð¾Ð»ÐµÐ¼ Ð½Ðµ Ð²ÑÑÐ²Ð»ÐµÐ½Ð¾.
Super-massive black hole wake or bulgeless edge-on galaxy?
Creators: name: Almeida, Jorge Sanchez
name: Montes, Mireia
name: Trujillo, Ignacio
Publisher: name: arXiv
Year: 2023
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: van Dokkum et al. (2023) reported the serendipitous discovery of a thin linear object interpreted as the trail of star-forming regions left behind by a runaway supermassive black hole (SMBH) kicked out from the center of a galaxy. Despite the undeniable interest in the idea, the actual physical interpretation is not devoid of difficulty. The wake of a SMBH produces only small perturbations on the external medium, which has to be in exceptional physical conditions to collapse gravitationally and form a long (40 kpc) massive (3e9 Msun) stellar trace in only 39 Myr. Here we offer a more conventional explanation: the stellar trail is a bulgeless galaxy viewed edge-on. This interpretation is supported by the fact that its position--velocity curve resembles a rotation curve which, together with its stellar mass, puts the object right on top of the Tully-Fisher relation characteristic of disk galaxies. Moreover, the rotation curve (Vmax sim 110 km/s), stellar mass, extension, width (z0 sim 1.2 kpc), and surface brightness profile of the object are very much like those of IC5249, a well-known local bulgeless edge-on galaxy. These observational facts are difficult to interpret within the SMBH wake scenario. We discuss in detail the pros and cons of the two options.
description: Accepted for publication in A&A Letters
title: Ð¡Ð¾Ð·Ð´Ð°Ð½Ð¸Ðµ ÑÐµÑÐ¸ Ð°Ð²ÑÐ¾Ð»Ð°Ð²Ð¾Ðº Ð¿Ð¾ Ð¿ÑÐ¾Ð¸Ð·Ð²Ð¾Ð´ÑÑÐ²Ñ Ð¸ Ð¿ÑÐ¾Ð´Ð°Ð¶Ðµ Ð¼ÑÐ³ÐºÐ¾Ð³Ð¾ Ð¼Ð¾ÑÐ¾Ð¶ÐµÐ½Ð¾Ð³Ð¾ (Ð½Ð° Ð¿ÑÐ¸Ð¼ÐµÑÐµ ÐÐ ÐÐ¸ÐºÐºÐµÑ Ð. Ð­.)
title: Ð±Ð°ÐºÐ°Ð»Ð°Ð²ÑÑÐºÐ°Ñ ÑÐ°Ð±Ð¾ÑÐ°
titleType: Subtitle
Creators: name: ÐÐ¸ÐºÐºÐµÑ, ÐÑÑÐµÐ¼
Publisher: name: Ð¡Ð°Ð½ÐºÑ-ÐÐµÑÐµÑÐ±ÑÑÐ³ÑÐºÐ¸Ð¹ Ð¿Ð¾Ð»Ð¸ÑÐµÑÐ½Ð¸ÑÐµÑÐºÐ¸Ð¹ ÑÐ½Ð¸Ð²ÐµÑÑÐ¸ÑÐµÑ ÐÐµÑÑÐ° ÐÐµÐ»Ð¸ÐºÐ¾Ð³Ð¾
Year: 2016
Subjects: Ð¼ÑÐ³ÐºÐ¾Ðµ Ð¼Ð¾ÑÐ¾Ð¶ÐµÐ½Ð¾Ðµ
Ð°Ð²ÑÐ¾Ð»Ð°Ð²ÐºÐ¸
Ð»Ð¾Ð³Ð¸ÑÑÐ¸ÑÐµÑÐºÐ°Ñ Ð´ÐµÑÑÐµÐ»ÑÐ½Ð¾ÑÑÑ
Ð·Ð°ÐºÑÐ¿ÐºÐ¸
soft ice cream
mobile shops
logistic activities
purchase

description: Ð Ð±Ð°ÐºÐ°Ð»Ð°Ð²ÑÑÐºÐ¾Ð¹ ÑÐ°Ð±Ð¾ÑÐµ ÑÐ°ÑÑÐ¼Ð¾ÑÑÐµÐ½Ð° Ð¿ÑÐ¾Ð±Ð»ÐµÐ¼Ð°, Ð²ÑÑÐ²Ð»ÐµÐ½Ð½Ð°Ñ Ð² ÑÐ¾Ð´Ðµ Ð¿ÑÐ¾ÑÐ¾Ð¶Ð´ÐµÐ½Ð¸Ñ Ð¿ÑÐµÐ´Ð´Ð¸Ð¿Ð»Ð¾Ð¼Ð½Ð¾Ð¹ Ð¿ÑÐ°ÐºÑÐ¸ÐºÐ¸, Ð¿ÑÐµÐ´ÑÑÐ°Ð²Ð»ÐµÐ½Ñ Ð²Ð°ÑÐ¸Ð°Ð½ÑÑ ÐµÐµ ÑÐµÑÐµÐ½Ð¸Ñ Ð¸ ÑÐ°ÑÑÑÐ¸ÑÐ°Ð½Ñ Ð´Ð¾ÑÐ¾Ð´Ñ, ÑÐ°ÑÑÐ¾Ð´Ñ Ð¸ Ð½Ð°Ð»Ð¾Ð³Ð¸ ÐÐ, Ð²Ð»Ð¸ÑÑÑÐ¸Ðµ Ð½Ð° ÑÐµÑÐµÐ½Ð¸Ðµ Ð´Ð°Ð½Ð½Ð¾Ð¹ Ð¿ÑÐ¾Ð±Ð»ÐµÐ¼Ñ. ÐÑÐµÐ´Ð»Ð°Ð³Ð°ÐµÑÑÑ ÑÐ¾Ð·Ð´Ð°ÑÑ ÑÐµÑÑ Ð´Ð»Ñ Ð¿Ð¾Ð»ÑÑÐµÐ½Ð¸Ñ Ð±Ð¾Ð»ÑÑÐµÐ¹ Ð²ÑÑÑÑÐºÐ¸. Ð¢Ð°Ðº Ð¶Ðµ ÑÐ°ÑÑÐ¸ÑÐµÐ½Ð¸Ðµ Ð¿ÑÐµÐ´Ð¿ÑÐ¸ÑÑÐ¸Ñ ÑÐ¿Ð¾ÑÐ¾Ð±ÑÑÐ²ÑÐµÑ Ð¼Ð¸Ð½Ð¸Ð¼Ð¸Ð·Ð°ÑÐ¸Ð¸ Ð·Ð°ÑÑÐ°Ñ.
description: The bachelor work has been considered a problem, identified during the passage of pre-diploma practice, ways to solve the problems are designed technical and economic parameters influencing the solution to this problem. Establishment of a retail chain to get more revenue. Also, the expansion of the company helps to minimize costs.
Zusatzdokumente für "Leitfaden für den ortsflexiblen Einsatz von kollaborativen Robotern"
Creators: name: Härdtlein, Christian
name: Hillgartner, Laura
name: Berger, Julia
Publisher: name: Fraunhofer-Gesellschaft
Year: 2022
Subjects: subject: DDC::600 Technik, Medizin, angewandte Wissenschaften::620 Ingenieurwissenschaften::629 Andere Fachrichtungen der Ingenieurwissenschaften

description: Ergänzende Informationen (u. a. Vorlagen, Checklisten) und Hilfsdokumente für den "Leitfaden für den ortsflexiblen Einsatz von kollaborativen Robotern".
Constraints on the $e^{\pm }$ Pair Injection of Pulsar Halos: Implications from the Galactic Diffuse Multi-TeV Gamma-ray Emission
Creators: name: Yan, Kai
name: Liu, Ruo-Yu
Publisher: name: arXiv
Year: 2023
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: Diffuse gamma-ray emission (DGE) has been discovered over the Galactic disk in the energy range from sub-GeV to sub-PeV. While it is believed to be dominated by the pionic emission of cosmic ray (CR) hadrons via interactions with interstellar medium, unresolved gamma-ray sources may also be potential contributors. TeV gamma-ray halos around middle-aged pulsars have been proposed as such sources. Their contribution to DGE, however, highly depends on the injection rate of electrons and the injection spectral shape, which are not well determined based on current observations. The measured fluxes of DGE can thus provide constraints on the $e^\pm$ injection of the pulsar halo population in turn. In this paper, we estimate the contribution of pulsar halos to DGE based on the ATNF pulsar samples with taking into account the off-beamed pulsars. The recent measurement on DGE by Tibet AS$γ$ and an early measurement by MILAGRO are used to constrain the pair injection parameters of the pulsar halo population. Our result may be used to distinguish different models for pulsar halos.
description: 18 pages, 8 figures, 1 table. Accepted for publication in Physical Review D
Onthophagus marginatus
Creators: name: Kohlmann, Bert
name: Solís, Ángel
Publisher: name: Zenodo
Year: 2025
Subjects: Biodiversity
Taxonomy
Animalia
Arthropoda
Insecta
Coleoptera
Scarabaeidae
Onthophagus
Onthophagus marginatus

description: Onthophagus marginatus species group*. This
group is diagnosed by a pale antennal club; head frons with a strong carina; elytral intervals having a median row of tubercles each bearing a strong seta; distal edges of the elytra have contrasting pale markings (brown in O. fragosus); the pygidium has distinct setiferous umbilicate punctures; males with a brush of fused long hair at the distal end of the protibiae. Its two species live in Cuba.
Although no species of this group could be included in the mtDNA analysis, this aggregation is established based on a characteristic set of morphological characters mentioned in the diagnosis. The group is composed at present by O. marginatus Laporte and O. fragosus Génier & Howden. The first species is widely distributed on the island; the second has been collected in litter on an isolated patch of moist forest (650-935 m a.s.l.) (Matthews 1966; Génier & Howden 2014).
There is also a third species in the Greater Antilles living in Hispaniola, O. albicornis Palisot. Matthews (1966) is of the opinion that the species of the Greater Antilles are derived from a common ancestor. This might be so because O. albicornis shares with the two Cuban species the following characters: distal edges of the elytra have contrasting pale markings (brown in O. fragosus); the antennal clubs are white while alive, turning yellowish when dead; prominent brush of fused setae emerging from the distal end of the male foretibia. Génier and Howden (2014) indicated that the protibiae of O. fragosus lacked the apical setal brush. However, photographs provided by Andrew Smith of the male O. fragosus clearly shows the existence of this structure.
description: Published as part of Kohlmann, Bert & Solís, Ángel, 2025, A review of the species groups of the Western Hemisphere Onthophagus Latreille (Coleoptera: Scarabaeidae: Scarabaeinae) using COI barcoding and gene trees, pp. 401-447 in Zootaxa 5604 (4) on page 428, DOI: 10.11646/zootaxa.5604.4.1, http://zenodo.org/record/15213967
Testing angular momentum transport processes with asteroseismology of solar-type main-sequence stars
Creators: name: Bétrisey, Jérôme
name: Eggenberger, Patrick
name: Buldgen, Gaël
name: Benomar, Othman
name: Bazot, Michaël
Publisher: name: arXiv
Year: 2023
Subjects: subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences

description: Asteroseismology has become a powerful tool to study the internal rotation of stars, and its study allows to constrain the internal AM transport processes and better understand their physical nature. In this context, we compared the rotation rates predicted by asteroseismology and by starspots measurements for four main-sequence stars from the Kepler LEGACY sample, considering different AM transport prescriptions, and investigated if some of these prescriptions could be ruled out. We decoupled the modelling of the structure and of the rotational profile, respectively obtained by an asteroseismic characterization and by using rotating models including a detailed treatment of the AM transport. We then compared the mean asteroseismic rotation rate with the surface rotation rate from starspots measurements for each of the AM transport prescriptions. In the hotter part of the HRD (M > ~ 1.2Msun), combining asteroseismic constraints from splittings of pressure modes and surface rotation rates does not allow to conclude on the need for an efficient AM transport in addition to the sole transport by meridional circulation and shear instability. Both prescriptions are indeed consistent with the quasi-solid rotation measured by Benomar et al. (2015) and Nielsen et al. (2017). In the colder part of the HRD, the situation is different due to the efficient braking of the stellar surface by magnetised winds. We find a clear disagreement between the rotational properties of models including only hydrodynamic processes and asteroseismic constraints, while models with magnetic fields correctly reproduce the observations, similarly to the solar case. This shows the existence of a mass regime corresponding to main-sequence stars around ~ 6000 - 6200 K for which it is difficult to constrain the AM transport processes, unlike for hotter, Gamma Dor stars or colder, less massive solar analogs.
description: Accepted for publication as a Letter in Astronomy and Astrophysics, section 1. Letters to the Editor
title: Ð§Ð¸ÑÐ»ÐµÐ½Ð½Ð¾Ðµ Ð¼Ð¾Ð´ÐµÐ»Ð¸ÑÐ¾Ð²Ð°Ð½Ð¸Ðµ ÑÑÑÐ±ÑÐ»ÐµÐ½ÑÐ½Ð¾Ð¹ ÑÐ²Ð¾Ð±Ð¾Ð´Ð½Ð¾Ð¹ ÐºÐ¾Ð½Ð²ÐµÐºÑÐ¸Ð¸ Ð² ÑÐ¸Ð»Ð¸Ð½Ð´ÑÐ¸ÑÐµÑÐºÐ¸Ñ ÐµÐ¼ÐºÐ¾ÑÑÑÑ , Ð²ÐºÐ»ÑÑÐ°Ñ ÑÑÑÐµÐºÑÑ Ð²ÑÐ°ÑÐµÐ½Ð¸Ñ Ð¸ ÑÐ¾Ð¿ÑÑÐ¶ÐµÐ½Ð½Ð¾Ð³Ð¾ ÑÐµÐ¿Ð»Ð¾Ð¾Ð±Ð¼ÐµÐ½Ð°
title: ÑÐ¿ÐµÑÐ¸Ð°Ð»ÑÐ½Ð¾ÑÑÑ 01.02.05 "ÐÐµÑ Ð°Ð½Ð¸ÐºÐ° Ð¶Ð¸Ð´ÐºÐ¾ÑÑÐ¸, Ð³Ð°Ð·Ð° Ð¸ Ð¿Ð»Ð°Ð·Ð¼Ñ"
titleType: Subtitle
Creators: name: Ð¡Ð¼Ð¸ÑÐ½Ð¾Ð², Ð¡ÐµÑÐ³ÐµÐ¹
Publisher: name: Ð¡Ð°Ð½ÐºÑ-ÐÐµÑÐµÑÐ±ÑÑÐ³ÑÐºÐ¸Ð¹ Ð¿Ð¾Ð»Ð¸ÑÐµÑÐ½Ð¸ÑÐµÑÐºÐ¸Ð¹ ÑÐ½Ð¸Ð²ÐµÑÑÐ¸ÑÐµÑ ÐÐµÑÑÐ° ÐÐµÐ»Ð¸ÐºÐ¾Ð³Ð¾
Year: 2020
Subjects: Ð¢ÑÑÐ±ÑÐ»ÐµÐ½ÑÐ½Ð¾Ðµ ÑÐµÑÐµÐ½Ð¸Ðµ Ð² ÑÑÑÐ±Ð°Ñ
Ð¢ÑÑÐ±ÑÐ»ÐµÐ½ÑÐ½Ð¾Ðµ ÑÐµÑÐµÐ½Ð¸Ðµ
Ð¢ÐµÐ¿Ð»Ð¾Ð¾Ð±Ð¼ÐµÐ½ ÐºÐ¾Ð½Ð²ÐµÐºÑÐ¸Ð²Ð½ÑÐ¹
Ð§Ð¸ÑÐ»ÐµÐ½Ð½ÑÐµ Ð¼ÐµÑÐ¾Ð´Ñ

description: Ð Ð´Ð¸ÑÑÐµÑÑÐ°ÑÐ¸Ð¸ Ð¸Ð·Ð»Ð°Ð³Ð°ÑÑÑÑ ÑÐµÐ·ÑÐ»ÑÑÐ°ÑÑ Ð² Ð¾Ð±Ð»Ð°ÑÑÐ¸ ÑÐ¸ÑÐ»ÐµÐ½Ð½Ð¾Ð³Ð¾ Ð¼Ð¾Ð´ÐµÐ»Ð¸ÑÐ¾Ð²Ð°Ð½Ð¸Ñ ÑÑÑÐ±ÑÐ»ÐµÐ½ÑÐ½Ð¾Ð¹ ÑÐ²Ð¾Ð±Ð¾Ð´Ð½Ð¾Ð¹ ÐºÐ¾Ð½Ð²ÐµÐºÑÐ¸Ð¸ Ð² ÑÐ¸Ð»Ð¸Ð½Ð´ÑÐ¸ÑÐµÑÐºÐ¸Ñ ÐµÐ¼ÐºÐ¾ÑÑÑÑ, Ð²ÐºÐ»ÑÑÐ°Ñ ÑÑÑÐµÐºÑÑ Ð²ÑÐ°ÑÐµÐ½Ð¸Ñ Ð¸ ÑÐ¾Ð¿ÑÑÐ¶ÐµÐ½Ð½Ð¾Ð³Ð¾ ÑÐµÐ¿Ð»Ð¾Ð¾Ð±Ð¼ÐµÐ½Ð°. Ð ÑÐ°ÑÑÐ½Ð¾ÑÑÐ¸, Ð² Ð½ÐµÐ¹ Ð¿ÑÐµÐ´ÑÑÐ°Ð²Ð»ÐµÐ½Ñ ÑÐµÐ·ÑÐ»ÑÑÐ°ÑÑ Ð¿ÑÐ¸Ð¼ÐµÐ½ÐµÐ½Ð¸Ñ ÑÐ°Ð·Ð»Ð¸ÑÐ½ÑÑ Ð²ÑÑÐ¸ÑÐ»Ð¸ÑÐµÐ»ÑÐ½ÑÑ Ð¿Ð¾Ð´ÑÐ¾Ð´Ð¾Ð² Ð´Ð»Ñ ÑÐ¸ÑÐ»ÐµÐ½Ð½Ð¾Ð³Ð¾ Ð¼Ð¾Ð´ÐµÐ»Ð¸ÑÐ¾Ð²Ð°Ð½Ð¸Ñ ÑÑÑÐ±ÑÐ»ÐµÐ½ÑÐ½ÑÑ ÑÐµÐ¶Ð¸Ð¼Ð¾Ð² ÑÐ²Ð¾Ð±Ð¾Ð´Ð½Ð¾Ð¹ ÐºÐ¾Ð½Ð²ÐµÐºÑÐ¸Ð¸ Ð ÑÐ»ÐµÑ-ÐÐµÐ½Ð°ÑÐ° Ð² ÑÑÐ°ÑÐ¸Ð¾Ð½Ð°ÑÐ½Ð¾Ð¹ Ð¸ Ð²ÑÐ°ÑÐ°ÑÑÐµÐ¹ÑÑ ÑÐ¸Ð»Ð¸Ð½Ð´ÑÐ¸ÑÐµÑÐºÐ¾Ð¹ ÐµÐ¼ÐºÐ¾ÑÑÐ¸ Ð¿ÑÐ¸ ÑÐ°Ð·Ð»Ð¸ÑÐ½ÑÑ Ð·Ð½Ð°ÑÐµÐ½Ð¸ÑÑ Ð¾Ð¿ÑÐµÐ´ÐµÐ»ÑÑÑÐ¸Ñ Ð¿Ð°ÑÐ°Ð¼ÐµÑÑÐ¾Ð² Ð·Ð°Ð´Ð°ÑÐ¸ (ÑÐ¸ÑÐ»Ð°Ñ ÐÑÐ°Ð½Ð´ÑÐ»Ñ, Ð ÑÐ»ÐµÑ Ð¸ Ð Ð¾ÑÑÐ±Ð¸). ÐÐ°ÑÑÐ´Ñ Ñ ÑÑÐ¸Ð¼, Ð² Ð´Ð¸ÑÑÐµÑÑÐ°ÑÐ¸Ð¸ ÑÐ¸ÑÐ»ÐµÐ½Ð½Ð¾ Ð¸ÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð¾ Ð²Ð»Ð¸ÑÐ½Ð¸Ðµ ÐºÐ¾Ð½Ð´ÑÐºÑÐ¸Ð²Ð½Ð¾Ð³Ð¾ ÑÐµÐ¿Ð»Ð¾Ð¿ÐµÑÐµÐ½Ð¾ÑÐ° Ð² Ð³Ð¾ÑÐ¸Ð·Ð¾Ð½ÑÐ°Ð»ÑÐ½ÑÑ ÑÑÐµÐ½ÐºÐ°Ñ ÐºÐ¾Ð½ÐµÑÐ½Ð¾Ð¹ ÑÐ¾Ð»ÑÐ¸Ð½Ñ Ð½Ð° ÑÑÑÑÐºÑÑÑÑ ÑÑÑÐ±ÑÐ»ÐµÐ½ÑÐ½Ð¾Ð¹ ÐºÐ¾Ð½Ð²ÐµÐºÑÐ¸Ð¸ ÑÑÑÑÐ¸ Ð¸ ÐºÐ¾Ð½Ð²ÐµÐºÑÐ¸Ð²Ð½ÑÐ¹ ÑÐµÐ¿Ð»Ð¾Ð¿ÐµÑÐµÐ½Ð¾Ñ Ð² ÑÑÐ°ÑÐ¸Ð¾Ð½Ð°ÑÐ½Ð¾Ð¹ Ð¸ Ð²ÑÐ°ÑÐ°ÑÑÐµÐ¹ÑÑ ÑÐ¸Ð»Ð¸Ð½Ð´ÑÐ¸ÑÐµÑÐºÐ¾Ð¹ ÐµÐ¼ÐºÐ¾ÑÑÐ¸.
Quantum Hall effect near the charge neutrality point in two-dimensional electron-hole system
Creators: name: Gusev, G. M.
name: Olshanetsky, E. B.
name: Kvon, Z. D.
name: Mikhailov, N. N.
name: Dvoretsky, S. A.
name: Portal, J. C.
Publisher: name: arXiv
Year: 2010
Subjects: subject: Mesoscale and Nanoscale Physics (cond-mat.mes-hall)
subject: FOS: Physical sciences

description: We study the transport properties of $HgTe$-based quantum wells containing simultaneously electrons and holes in magnetic field B. At the charge neutrality point (CNP) with nearly equal electron and hole densities, the resistance is found to increase very strongly with B while the Hall resistivity turns to zero. This behavior results in a wide plateau in the Hall conductivity $σ_{xy}\approx 0$ and in a minimum of diagonal conductivity $σ_{xx}$ at $ν=ν_p-ν_n=0$, where $ν_n$ and $ν_p$ are the electron and hole Landau filling factors. We suggest that the transport at the CNP point is determined by electron-hole "snake states" propagating along the $ν=0$ lines. Our observations are qualitatively similar to the quantum Hall effect in graphene as well as to the transport in random magnetic field with zero mean value.
description: 4.5 pages, 4 figures
title: ÐÐ¾Ð½Ð´ÐµÐ½ÑÐ°ÑÐ¾ÑÐ½Ð°Ñ ÑÐµÑ Ð½Ð¸ÐºÐ°. Ð­Ð»ÐµÐºÑÑÐ¾ÑÐ¸Ð·Ð¸ÑÐµÑÐºÐ¸Ðµ Ð¿ÑÐ¾ÑÐµÑÑÑ Ð² ÑÐ»ÐµÐºÑÑÐ¸ÑÐµÑÐºÐ¸Ñ ÐºÐ¾Ð½Ð´ÐµÐ½ÑÐ°ÑÐ¾ÑÐ°Ñ
title: ÑÑÐµÐ±Ð½Ð¾Ðµ Ð¿Ð¾ÑÐ¾Ð±Ð¸Ðµ
titleType: Subtitle
Creators: name: ÐÐµÐ»ÑÐºÐ¾, ÐÐ¸ÐºÑÐ¾Ñ
name: ÐÐ¼ÐµÐ»ÑÑÐ½Ð¾Ð², ÐÐ»ÐµÐ³
name: ÐÐ²Ð°Ð½Ð¾Ð², ÐÐ²Ð°Ð½
name: ÐÐ»Ð¾ÑÐ½Ð¸ÐºÐ¾Ð², ÐÐ½Ð´ÑÐµÐ¹
Publisher: name: ÐÐÐÐÐ¢ÐÐ¥-ÐÐ ÐÐ¡Ð¡
Year: 2019
Subjects: Ð­Ð»ÐµÐºÑÑÐ¸ÑÐµÑÐºÐ¸Ðµ ÐºÐ¾Ð½Ð´ÐµÐ½ÑÐ°ÑÐ¾ÑÑ

description: Ð¡Ð¾Ð¾ÑÐ²ÐµÑÑÑÐ²ÑÐµÑ ÑÐ¾Ð´ÐµÑÐ¶Ð°Ð½Ð¸Ñ ÑÐ¿ÐµÑÐ¸Ð°Ð»ÑÐ½Ð¾ÑÑÐ¸ 05.09.02 Â«Ð­Ð»ÐµÐºÑÑÐ¾ÑÐµÑÐ½Ð¸ÑÐµÑÐºÐ¸Ðµ
Ð¼Ð°ÑÐµÑÐ¸Ð°Ð»Ñ Ð¸ Ð¸Ð·Ð´ÐµÐ»Ð¸ÑÂ».
Ð ÑÐµÐ·ÑÐ»ÑÑÐ°ÑÐµ Ð¸Ð·ÑÑÐµÐ½Ð¸Ñ Ð´Ð°Ð½Ð½Ð¾Ð³Ð¾ ÑÑÐµÐ±Ð½Ð¾Ð³Ð¾ Ð¿Ð¾ÑÐ¾Ð±Ð¸Ñ ÑÑÑÐ´ÐµÐ½ÑÑ Ð¿ÑÐ¸Ð¾Ð±ÑÐµÑÐ°ÑÑ
Ð¿ÑÐ¾ÑÐµÑÑÐ¸Ð¾Ð½Ð°Ð»ÑÐ½ÑÐµ ÐºÐ¾Ð¼Ð¿ÐµÑÐµÐ½ÑÐ¸Ð¸ Ð² Ð¾Ð±Ð»Ð°ÑÑÐ¸ ÑÐ»ÐµÐºÑÑÐ¸ÑÐµÑÐºÐ¾Ð³Ð¾ ÐºÐ¾Ð½Ð´ÐµÐ½ÑÐ°ÑÐ¾ÑÐ¾ÑÑÑÐ¾ÐµÐ½Ð¸Ñ, Ð° Ð¸Ð¼ÐµÐ½Ð½Ð¾: Ð·Ð½Ð°Ð½Ð¸Ðµ ÑÐ»ÐµÐºÑÑÐ¾ÑÐ¸Ð·Ð¸ÑÐµÑÐºÐ¸Ñ Ð¸ ÑÐµÐ¿Ð»Ð¾ÑÐ¸Ð·Ð¸ÑÐµÑÐºÐ¸Ñ ÑÐ²Ð¾Ð¹ÑÑÐ²
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Ð¿ÐµÑÑÐ¿ÐµÐºÑÐ¸Ð² ÑÐ°Ð·Ð²Ð¸ÑÐ¸Ñ Ð¸Ð·ÑÑÐ°ÐµÐ¼ÑÑ Ð¸Ð·Ð´ÐµÐ»Ð¸Ð¹ Ð½Ð° Ð¼Ð¸ÑÐ¾Ð²Ð¾Ð¼ ÑÑÐ½ÐºÐµ; Ð¿Ð¾Ð½Ð¸Ð¼Ð°Ð½Ð¸Ðµ ÑÐ¾Ð³Ð¾,
ÐºÐ°Ðº ÑÐ»ÐµÐºÑÑÐ¾ÑÐ¸Ð·Ð¸ÑÐµÑÐºÐ¸Ðµ Ð¿ÑÐ¾ÑÐµÑÑÑ Ð² ÐºÐ¾Ð½Ð´ÐµÐ½ÑÐ°ÑÐ¾ÑÐ°Ñ Ð²Ð»Ð¸ÑÑÑ Ð½Ð° ÐºÐ¾Ð½ÑÑÑÑÐºÑÐ¸Ñ,
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ÑÐºÑÐ¿Ð»ÑÐ°ÑÐ°ÑÐ¸Ð¸ ÑÐ¾Ð²ÑÐµÐ¼ÐµÐ½Ð½Ð¾Ð³Ð¾ Ð¾Ð±Ð¾ÑÑÐ´Ð¾Ð²Ð°Ð½Ð¸Ñ Ð¸ Ð¿ÑÐ¸Ð±Ð¾ÑÐ¾Ð².
Ð£ÑÐµÐ±Ð½Ð¾Ðµ Ð¿Ð¾ÑÐ¾Ð±Ð¸Ðµ Ð¼Ð¾Ð¶ÐµÑ Ð¸ÑÐ¿Ð¾Ð»ÑÐ·Ð¾Ð²Ð°ÑÑÑÑ ÑÑÑÐ´ÐµÐ½ÑÐ°Ð¼Ð¸, Ð¸Ð·ÑÑÐ°ÑÑÐ¸Ð¼Ð¸ Ð´Ð¸ÑÑÐ¸Ð¿Ð»Ð¸Ð½Ñ Â«ÐÐ¾Ð½Ð´ÐµÐ½ÑÐ°ÑÐ¾ÑÐ½Ð°Ñ ÑÐµÑÐ½Ð¸ÐºÐ°Â» Ð² ÑÐ°Ð¼ÐºÐ°Ñ Ð½Ð°Ð¿ÑÐ°Ð²Ð»ÐµÐ½Ð¸Ñ 13.04.02 Â«Ð­Ð»ÐµÐºÑÑÐ¾-
ÑÐ½ÐµÑÐ³ÐµÑÐ¸ÐºÐ° Ð¸ ÑÐ»ÐµÐºÑÑÐ¾ÑÐµÑÐ½Ð¸ÐºÐ°Â».
title: ÐÐ¾ÑÐºÐ¾Ð²ÑÐºÐ°Ñ Ð±Ð¸ÑÐ²Ð°: ÑÐµÐ½Ð¾Ð¼ÐµÐ½ ÐÑÐ¾ÑÐ¾Ð¹ Ð¼Ð¸ÑÐ¾Ð²Ð¾Ð¹
Creators: name: ÐÐµÐ²Ð·Ð¾ÑÐ¾Ð², ÐÐ¾ÑÐ¸Ñ
Publisher: name: Ð¡Ð¸ÐÐ¸ÐÑÐµÑÑ
Year: 2001
Subjects: Ð±Ð¸ÑÐ²Ñ Ð¸ ÑÑÐ°Ð¶ÐµÐ½Ð¸Ñ
ÐÑÐ¾ÑÐ°Ñ Ð¼Ð¸ÑÐ¾Ð²Ð°Ñ Ð²Ð¾Ð¹Ð½Ð°

description: ÐÐ½Ð¸Ð³Ð° Ð¿Ð¾ÑÐ²ÑÑÐµÐ½Ð° Ð³Ð»Ð°Ð²Ð½Ð¾Ð¹ Ð±Ð¸ÑÐ²Ðµ Ð²ÑÐ¾ÑÐ¾Ð¹ Ð¼Ð¸ÑÐ¾Ð²Ð¾Ð¹ Ð²Ð¾Ð¹Ð½Ñ, ÑÐ¾ÑÐ²Ð°Ð²ÑÐµÐ¹ Ð±ÑÐµÐ´Ð¾Ð²ÑÐµ Ð¿Ð»Ð°Ð½Ñ Ð³Ð¸ÑÐ»ÐµÑÐ¾Ð²ÑÐµÐ² Ð·Ð°ÐºÐ¾Ð½ÑÐ¸ÑÑ ÑÐ²Ð¾Ð¹ Â«Ð²Ð¾ÑÑÐ¾ÑÐ½ÑÐ¹ Ð¿Ð¾ÑÐ¾Ð´Â» Ð² ÑÑÑÑÐºÐ¾Ð¹ ÑÑÐ¾Ð»Ð¸ÑÐµ Ð¸ Ð·Ð°ÑÐµÐ¼ ÑÑÑÐ°Ð½Ð¾Ð²Ð¸ÑÑ Ð³Ð¾ÑÐ¿Ð¾Ð´ÑÑÐ²Ð¾ Ð½Ð°Ð´ Ð²ÑÐµÐ¼ Ð¼Ð¸ÑÐ¾Ð¼. Ð Ð½ÐµÐ¹ Ð¸Ð·Ð»Ð¾Ð¶ÐµÐ½Ñ Ð²ÑÐµ Ð¾ÑÐ½Ð¾Ð²Ð½ÑÐµ ÑÑÐ°Ð¿Ñ ÐÐ¾ÑÐºÐ¾Ð²ÑÐºÐ¾Ð¹ Ð±Ð¸ÑÐ²Ñ, Ð²Ð¿ÐµÑÐ²ÑÐµ Ð¿Ð¾Ð´ÑÐ¾Ð±Ð½Ð¾ Ð¾ÑÐ²ÐµÑÐ°ÑÑÑÑ Ð¼Ð°Ð»Ð¾Ð¸Ð·Ð²ÐµÑÑÐ½ÑÐµ ÑÐ°ÐºÑÑ, Ð´Ð°Ð½Ñ Ð¾ÑÐ²ÐµÑÑ Ð½Ð° Ð´Ð¸ÑÐºÑÑÑÐ¸Ð¾Ð½Ð½ÑÐµ Ð¸ ÑÐ¿Ð¾ÑÐ½ÑÐµ Ð²Ð¾Ð¿ÑÐ¾ÑÑ Ñ Ð½Ð¾Ð²ÑÐ¼Ð¸ Ð¾ÑÐµÐ½ÐºÐ°Ð¼Ð¸ ÑÐ¾Ð±ÑÑÐ¸Ð¹, Ð´Ð¾ÐºÑÐ¼ÐµÐ½ÑÐ¾Ð², ÑÐµÑÐµÐ½Ð¸Ð¹ Ð¸ Ð´ÐµÐ¹ÑÑÐ²Ð¸Ð¹ Ð¾ÑÐ´ÐµÐ»ÑÐ½ÑÑ Ð²Ð¾ÐµÐ½Ð°ÑÐ°Ð»ÑÐ½Ð¸ÐºÐ¾Ð²; Ð¿ÑÐ¸Ð²ÐµÐ´ÐµÐ½Ñ ÑÐµÐ·ÑÐ»ÑÑÐ°ÑÑ Ð¿Ð¾ÑÐ»ÐµÐ´Ð½Ð¸Ñ Ð¸ÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð¸Ð¹ Ð¾ ÑÐ¾ÑÑÐ°Ð²Ðµ ÑÐ¸Ð» Ð¸ ÑÑÐµÐ´ÑÑÐ² ÑÑÐ¾ÑÐ¾Ð½ Ð¸ Ð¸Ñ Ð¿Ð¾ÑÐµÑÑÑ Ð² Ð±Ð¸ÑÐ²Ðµ; Ð¿Ð¾ÐºÐ°Ð·Ð°Ð½Ñ Ð³ÐµÑÐ¾Ð¸Ð·Ð¼, ÑÑÐ¾Ð¹ÐºÐ¾ÑÑÑ ÑÐ¾Ð²ÐµÑÑÐºÐ¸Ñ Ð²Ð¾Ð¸Ð½Ð¾Ð² Ð¸ ÑÑÑÐ´Ð¾Ð²Ð¾Ð¹ Ð¿Ð¾Ð´Ð²Ð¸Ð³ Ð¶Ð¸ÑÐµÐ»ÐµÐ¹ ÑÑÐ¾Ð»Ð¸ÑÑ, Ð·Ð°ÑÐ¸ÑÐ¸Ð²ÑÐ¸Ñ ÐÐ¾ÑÐºÐ²Ñ. ÐÐ»Ñ Ð²ÑÐµÑ Ð¸Ð½ÑÐµÑÐµÑÑÑÑÐ¸ÑÑÑ Ð¸ÑÑÐ¾ÑÐ¸ÐµÐ¹ ÐÑÐµÑÐµÑÑÐ²Ð°.
CTK - A new CCD Camera at the University Observatory Jena
Creators: name: Mugrauer, M.
Publisher: name: arXiv
Year: 2009
Subjects: subject: Instrumentation and Methods for Astrophysics (astro-ph.IM)
subject: FOS: Physical sciences

description: The Cassegrain-Teleskop-Kamera (CTK) is a new CCD imager which is operated at the University Observatory Jena since begin of 2006. This article describes the main characteristics of the new camera. The properties of the CCD detector, the CTK image quality, as well as its detection limits for all filters are presented.
description: AN accepted, 6 pages, 15 figures, 2 tables
Stars on the edge: Galactic tides and the outskirts of the Sculptor dwarf spheroidal
Creators: name: Sestito, Federico
name: Roediger, Joel
name: Navarro, Julio F.
name: Jensen, Jaclyn
name: Venn, Kim A.
name: Smith, Simon E. T.
name: Hayes, Christian
name: McConnachie, Alan W.
Publisher: name: arXiv
Year: 2023
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences

description: The formation of "stellar halos" in dwarf galaxies have been discussed in terms of early mergers or Galactic tides, although fluctuations in the gravitational potential due to stellar feedback is also a possible candidate mechanism. A Bayesian algorithm is used to find new candidate members in the extreme outskirts of the Sculptor dwarf galaxy. Precise metallicities and radial velocities for two distant stars are measured from their spectra taken with the Gemini South GMOS spectrograph. The radial velocity, proper motion and metallicity of these targets are consistent with Sculptor membership. As a result, the known boundary of the Sculptor dwarf extends now out to an elliptical distance of $\sim10$ half-light radii, which corresponds to a projected physical distance of $\sim3$ kpc. As reported in earlier work, the overall distribution of radial velocities and metallicities indicate the presence of a more spatially and kinematically dispersed metal-poor population that surrounds the more concentrated and colder metal-rich stars. Sculptor's density profile shows a "kink" in its logarithmic slope at a projected distance of $\sim25$ arcmin (620 pc), which we interpret as evidence that Galactic tides have helped to populate the distant outskirts of the dwarf. We discuss further ways to test and validate this tidal interpretation for the origin of these distant stars.
description: Accepted for publication on MNRAS. Figure 1 now displays all the candidate members. arXiv admin note: text overlap with arXiv:2301.13214
Quasiregular singularities taken seriously
Creators: name: Krasnikov, Serguei
Publisher: name: arXiv
Year: 2009
Subjects: subject: General Relativity and Quantum Cosmology (gr-qc)
subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: FOS: Physical sciences

description: I discuss a special class of singularities obtained as a natural 4-dimensional generalization of the conical singularity. Such singularities (called quasiregular) are ruinous for the predictive force of general relativity, so one often assumes (implicitly as a rule) that they can be somehow excluded from the theory. In fact, however, attempts to do so (without forbidding the singularities by fiat) have failed so far. It is advisable therefore to explore the possibility that their existence is not prohibited after all. I argue that quasiregular singularities, if allowed, may appear either in situations where causality is endangered or in the early Universe. In the latter case objects might appear strongly (though not quite) resembling cosmic strings. Those objects would be observable and, moreover, it is not impossible that we already do observe one.
description: Lecture given at 5-th International School on Field Theory and Gravitation in Brazil
A new small glitch in Vela discovered with a hidden Markov model
Creators: name: Dunn, L.
name: Melatos, A.
name: Espinoza, C. M.
name: Antonopoulou, D.
name: Dodson, R.
Publisher: name: arXiv
Year: 2023
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: A striking feature of the Vela pulsar (PSR J0835$-$4510) is that it undergoes sudden increases in its spin frequency, known as glitches, with a fractional amplitude on the order of $10^{-6}$ approximately every 900 days. Glitches of smaller magnitudes are also known to occur in Vela. Their distribution in both time and amplitude is less well constrained but equally important for understanding the physical process underpinning these events. In order to better understand these small glitches in Vela, an analysis of high-cadence observations from the Mount Pleasant Observatory is presented. A hidden Markov model (HMM) is used to search for small, previously undetected glitches across 24 years of observations covering MJD 44929 to MJD 53647. One previously unknown glitch is detected around MJD 48636 (Jan 15 1992), with fractional frequency jump $Δf/f = (8.19 \pm 0.04) \times 10^{-10}$ and frequency derivative jump $Δ\dot{f}/\dot{f} = (2.98 \pm 0.01) \times 10^{-4}$. Two previously reported small glitches are also confidently re-detected, and independent estimates of their parameters are reported. Excluding these events, 90% confidence frequentist upper limits on the sizes of missed glitches are also set, with a median upper limit of $Δf^{90\%}/f = 1.35 \times 10^{-9}$. Upper limits of this kind are enabled by the semi-automated and computationally efficient nature of the HMM, and are crucial to informing studies which are sensitive to the lower end of the glitch size distribution.
description: 10 pages, 7 figures. Accepted for publication in Monthly Notices of the Royal Astronomical Society
title: Ð¡Ð¾Ð²ÐµÑÑÐµÐ½ÑÑÐ²Ð¾Ð²Ð°Ð½Ð¸Ðµ Ð¼Ð°ÑÐºÐµÑÐ¸Ð½Ð³Ð¾Ð²Ð¾Ð¹ Ð¿Ð¾Ð»Ð¸ÑÐ¸ÐºÐ¸ Ð¿ÑÐ¾Ð¸Ð·Ð²Ð¾Ð´ÑÑÐ²ÐµÐ½Ð½Ð¾Ð¹ Ð¾ÑÐ³Ð°Ð½Ð¸Ð·Ð°ÑÐ¸Ð¸ (Ð½Ð° Ð¿ÑÐ¸Ð¼ÐµÑÐµ ÐÐÐ Â«ÐÐÐ-ÐÐ¸ÑÐµÐ¹Ð½Ð¾Ðµ Ð¿ÑÐ¾Ð¸Ð·Ð²Ð¾Ð´ÑÑÐ²Ð¾Â»)
title: Ð¼Ð°Ð³Ð¸ÑÑÐµÑÑÐºÐ°Ñ Ð´Ð¸ÑÑÐµÑÑÐ°ÑÐ¸Ñ
titleType: Subtitle
Creators: name: Ð¯ÐºÐ¾Ð²Ð»ÐµÐ², ÐÐ¸ÑÐ¸Ð»Ð»
Publisher: name: Ð¡Ð°Ð½ÐºÑ-ÐÐµÑÐµÑÐ±ÑÑÐ³ÑÐºÐ¸Ð¹ Ð¿Ð¾Ð»Ð¸ÑÐµÑÐ½Ð¸ÑÐµÑÐºÐ¸Ð¹ ÑÐ½Ð¸Ð²ÐµÑÑÐ¸ÑÐµÑ ÐÐµÑÑÐ° ÐÐµÐ»Ð¸ÐºÐ¾Ð³Ð¾
Year: 2016
Subjects: ÐÐµÑÐ°Ð»Ð»ÑÑÐ³Ð¸ÑÐµÑÐºÐ¸Ðµ Ð·Ð°Ð²Ð¾Ð´Ñ
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Narrow loophole for H2-dominated atmospheres on habitable rocky planets around M dwarfs
Creators: name: Hu, Renyu
name: Gaillard, Fabrice
name: Kite, Edwin
Publisher: name: arXiv
Year: 2023
Subjects: subject: Earth and Planetary Astrophysics (astro-ph.EP)
subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences

description: Habitable rocky planets around M dwarfs that have H2-dominated atmospheres, if they exist, would permit characterizing habitable exoplanets with detailed spectroscopy using JWST, owing to their extended atmospheres and small stars. However, the H2-dominated atmospheres that are consistent with habitable conditions cannot be too massive, and a moderate-size H2-dominated atmosphere will lose mass to irradiation-driven atmospheric escape on rocky planets around M dwarfs. We evaluate volcanic outgassing and serpentinization as two potential ways to supply H2 and form a steady-state H2-dominated atmosphere. For rocky planets of 1-7 Earth mass and early, mid, and late M dwarfs, the expected volcanic outgassing rates from a reduced mantle fall short of the escape rates by >~1 order of magnitude, and a generous upper limit of the serpentinization rate is still less than the escape rate by a factor of a few. Special mechanisms that may sustain the steady-state H2-dominated atmosphere include direct interaction between liquid water and mantle, heat-pipe volcanism from a reduced mantle, and hydrodynamic escape slowed down by efficient upper-atmospheric cooling. It is thus unlikely to find moderate-size, H2-dominated atmospheres on rocky planets of M dwarfs that would support habitable environments.
description: Accepted for publication in ApJ Letters
String dynamics and ejection along the axis of a spinning black hole
Creators: name: Jacobson, Ted
name: Sotiriou, Thomas P.
Publisher: name: arXiv
Year: 2008
Subjects: subject: General Relativity and Quantum Cosmology (gr-qc)
subject: Astrophysics (astro-ph)
subject: High Energy Physics - Theory (hep-th)
subject: FOS: Physical sciences

description: Relativistic current carrying strings moving axisymmetrically on the background of a Kerr black hole are studied. The boundaries and possible types of motion of a string with a given energy and current are found. Regions of parameters for which the string falls into the black hole, or is trapped in a toroidal volume, or can escape to infinity, are identified, and representative trajectories are examined by numerical integration, illustrating various interesting behaviors. In particular, we find that a string can start out at rest near the equatorial plane and, after bouncing around, be ejected out along the axis, some of its internal (elastic or rotational kinetic) energy having been transformed into translational kinetic energy. The resulting velocity can be an order unity fraction of the speed of light. This process results from the presence of an outer tension barrier and an inner angular momentum barrier that are deformed by the gravitational field. We speculatively discuss the possible astrophysical significance of this mechanism as a means of launching a collimated jet of MHD plasma flux tubes along the spin axis of a gravitating system fed by an accretion disk.
description: 14 pages, 11 figures; v.2: minor edits, references added, typos corrected, published version
Classifying FRB spectrograms using nonlinear dimensionality reduction techniques
Creators: name: Yang, X.
name: Zhang, S. -B.
name: Wang, J. -S.
name: Wu, X. -F.
Publisher: name: arXiv
Year: 2023
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: Instrumentation and Methods for Astrophysics (astro-ph.IM)
subject: FOS: Physical sciences

description: Fast radio bursts (FRBs) are mysterious astronomical phenomena, and it is still uncertain whether they consist of multiple types. In this study we use two nonlinear dimensionality reduction algorithms - Uniform Manifold Approximation and Projection (UMAP) and t-distributed stochastic neighbour embedding (t-SNE) - to differentiate repeaters from apparently non-repeaters in FRBs. Based on the first Canadian Hydrogen Intensity Mapping Experiment (CHIME) FRB catalogue, these two methods are applied to standardized parameter data and image data from a sample of 594 sub-bursts and 535 FRBs, respectively. Both methods are able to differentiate repeaters from apparently non-repeaters. The UMAP algorithm using image data produces more accurate results and is a more model-independent method. Our result shows that in general repeater clusters tend to be narrowband, which implies a difference in burst morphology between repeaters and apparently non-repeaters. We also compared our UMAP predictions with the CHIME/FRB discovery of 6 new repeaters, the performance was generally good except for one outlier. Finally, we highlight the need for a larger and more complete sample of FRBs.
description: 10 pages, 9 figures, 4 tables, accepted by MNRAS
title: ÐÐµÐ¼ÐµÑÐºÐ¸Ð¹ ÑÐ·ÑÐº. ÐÑÐ°ÐºÑÐ¸ÐºÑÐ¼ Ð¿Ð¾ Ð°Ð½Ð°Ð»Ð¸ÑÐ¸ÑÐµÑÐºÐ¾Ð¼Ñ ÑÑÐµÐ½Ð¸Ñ. Ð£ÑÐ¾Ð²ÐµÐ½Ñ Ð2-Ð1
title: [ÑÑÐµÐ±Ð½Ð¾Ðµ Ð¿Ð¾ÑÐ¾Ð±Ð¸Ðµ]
titleType: Subtitle
Creators: name: ÐÑÐ»Ð¾Ð²Ð°, ÐÐ»ÑÐ³Ð°
name: ÐÐ°ÑÐ¸Ð½Ð°, ÐÑÐ´Ð¼Ð¸Ð»Ð°
Publisher: name: Ð¡Ð°Ð½ÐºÑ-ÐÐµÑÐµÑÐ±ÑÑÐ³ÑÐºÐ¸Ð¹ Ð¿Ð¾Ð»Ð¸ÑÐµÑÐ½Ð¸ÑÐµÑÐºÐ¸Ð¹ ÑÐ½Ð¸Ð²ÐµÑÑÐ¸ÑÐµÑ ÐÐµÑÑÐ° ÐÐµÐ»Ð¸ÐºÐ¾Ð³Ð¾
Year: 2021
Subjects: Ð½ÐµÐ¼ÐµÑÐºÐ¸Ð¹ ÑÐ·ÑÐº
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Ð»Ð¸Ð½Ð³Ð²Ð¸ÑÑÐ¸ÐºÐ°
ÑÑÐµÐ±Ð½Ð¸ÐºÐ¸ Ð¸ Ð¿Ð¾ÑÐ¾Ð±Ð¸Ñ Ð´Ð»Ñ Ð²ÑÐ·Ð¾Ð²

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Quaoar: A Rock in the Kuiper belt
Creators: name: Fraser, W. C.
name: Brown, M. E.
Publisher: name: arXiv
Year: 2010
Subjects: subject: Earth and Planetary Astrophysics (astro-ph.EP)
subject: FOS: Physical sciences

description: Here we report WFPC2 observations of the Quaoar-Weywot Kuiper belt binary. From these observations we find that Weywot is on an elliptical orbit with eccentricity of 0.14 {\pm} 0.04, period of 12.438 {\pm} 0.005 days, and a semi-major axis of 1.45 {\pm} 0.08 {\times} 104 km. The orbit reveals a surpsingly high Quaoar-Weywot system mass of 1.6{\pm}0.3{\times}10^21 kg. Using the surface properties of the Uranian and Neptunian satellites as a proxy for Quaoar's surface, we reanalyze the size estimate from Brown and Trujillo (2004). We find, from a mean of available published size estimates, a diameter for Quaoar of 890 {\pm} 70 km. We find Quaoar's density to be ρ= 4.2 {\pm} 1.3 g cm^-3, possibly the highest density in the Kuiper belt.
description: 11 pages, 2 figures, accepted for publication in ApJ letters.
title: Ð Ð°Ð·ÑÐ°Ð±Ð¾ÑÐºÐ° ÑÐµÑ Ð½Ð¾Ð»Ð¾Ð³Ð¸Ð¸ Ð¸Ð·Ð³Ð¾ÑÐ¾Ð²Ð»ÐµÐ½Ð¸Ñ ÑÐ¾ÑÑÐ´Ð° Ð¸Ð· ÑÐ¸ÑÐ°Ð½Ð¾Ð²Ð¾Ð³Ð¾ ÑÐ¿Ð»Ð°Ð²Ð° Ð¼Ð°ÑÐºÐ¸ ÐÐ¢1-0
title: Ð±Ð°ÐºÐ°Ð»Ð°Ð²ÑÑÐºÐ°Ñ ÑÐ°Ð±Ð¾ÑÐ°
titleType: Subtitle
Creators: name: ÐÐ°ÐºÐ°Ð´Ð¶Ð°Ð½Ð¾Ð² , Ð¢Ð¸Ð¼ÑÑ
Publisher: name: Ð¡Ð°Ð½ÐºÑ-ÐÐµÑÐµÑÐ±ÑÑÐ³ÑÐºÐ¸Ð¹ Ð¿Ð¾Ð»Ð¸ÑÐµÑÐ½Ð¸ÑÐµÑÐºÐ¸Ð¹ ÑÐ½Ð¸Ð²ÐµÑÑÐ¸ÑÐµÑ ÐÐµÑÑÐ° ÐÐµÐ»Ð¸ÐºÐ¾Ð³Ð¾
Year: 2017
Subjects: ÑÐ¸ÑÐ°Ð½Ð¾Ð²ÑÐµ ÑÐ¿Ð»Ð°Ð²Ñ
ÑÐ²Ð°ÑÐ¸Ð²Ð°ÐµÐ¼Ð¾ÑÑÑ
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ÑÐµÑ Ð½Ð¾Ð»Ð¾Ð³Ð¸Ñ ÑÐ²Ð°ÑÐºÐ¸ ÑÐ¸ÑÐ°Ð½Ð°

description: ÐÐ°Ð½Ð½Ð°Ñ ÑÐ°Ð±Ð¾ÑÐ° Ð¿Ð¾ÑÐ²ÑÑÐµÐ½Ð° Ð¿ÑÐ¾Ð±Ð»ÐµÐ¼Ðµ ÑÐ²Ð°ÑÐºÐ¸ ÑÐ¸ÑÐ°Ð½Ð¾Ð²ÑÑ ÑÐ¿Ð»Ð°Ð²Ð¾Ð². ÐÑÐ»Ð° ÑÐ°Ð·ÑÐ°Ð±Ð¾ÑÐ°Ð½Ð° ÑÐµÑÐ½Ð¾Ð»Ð¾Ð³Ð¸Ñ ÑÐ²Ð°ÑÐºÐ¸ ÑÐ¸ÑÐ°Ð½Ð¾Ð²Ð¾Ð³Ð¾ ÑÐ¾ÑÑÐ´Ð° Ð¸Ð· Ð¼Ð°ÑÐºÐ¸ ÐÐ¢1-0. ÐÑÐ¾Ð°Ð½Ð°Ð»Ð¸Ð·Ð¸ÑÐ¾Ð²Ð°Ð½Ñ Ð¾ÑÐ½Ð¾Ð²Ð½ÑÐµ Ð¿ÑÐ¾Ð±Ð»ÐµÐ¼Ñ, ÑÐ²ÑÐ·Ð°Ð½Ð½ÑÐµ ÑÐ¾ ÑÐ²Ð°ÑÐºÐ¾Ð¹ ÑÐ¸ÑÐ°Ð½Ð¾Ð²ÑÑ ÑÐ¿Ð»Ð°Ð²Ð¾Ð². ÐÐ°Ð´Ð°Ð½Ñ ÑÐµÐ¶Ð¸Ð¼Ñ ÑÐ²Ð°ÑÐºÐ¸, Ð¾Ð¿ÑÐµÐ´ÐµÐ»ÐµÐ½Ñ Ð²Ð¸Ð´Ñ ÑÐ°Ð·Ð´ÐµÐ»Ð¾Ðº ÐºÑÐ¾Ð¼Ð¾Ðº, Ð° ÑÐ°ÐºÐ¶Ðµ ÑÐ¿Ð¾ÑÐ¾Ð±Ñ Ð·Ð°ÑÐ¸ÑÑ Ð´Ð»Ñ Ð¿Ð¾Ð»ÑÑÐµÐ½Ð¸Ñ ÐºÐ°ÑÐµÑÑÐ²ÐµÐ½Ð½ÑÑ ÑÐ²Ð°ÑÐ½ÑÑ ÑÐ¾ÐµÐ´Ð¸Ð½ÐµÐ½Ð¸Ð¹.