cometadata/datacite-rtg-text-other-reclassification-records huggingface dataset:
Time variability of ultra-fast BAL outflows using SALT: C IV equivalent width analysis
Creators: name: Aromal, P.
name: Srianand, R.
name: Petitjean, P.
Publisher: name: arXiv
Year: 2023
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: We study the time variability (over $\le$7.3 yrs) of ultra-fast outflows (UFOs) detected in a sample of 64 C IV broad absorption line (BAL) quasars (with 80 distinct BAL components) monitored using the Southern African Large Telescope. By comparing the properties of the quasar in our sample with those of a control sample of non-BAL quasars we show that the distributions of black hole mass are different and the bolometric luminosities and optical photometric variations of UFO BAL quasars are slightly smaller compared to that of non-BAL quasars. The detection fraction of C IV equivalent width (W) variability ($\sim$95%), the fractional variability amplitude ($\frac{ΔW}{W}$) and the fraction of ``highly variable" BAL (i.e., |$\frac{ΔW}{W}$| $>$0.67) components ($\sim$ 33%) are higher in our sample compared to the general BAL population. The scatter in $\frac{ΔW}{W}$ and the fraction of ``highly variable" BALs increase with the time-scale probed. The $\frac{ΔW}{W}$ distribution is asymmetric at large time scales. We attribute this to the BAL strengthening time scales being shorter than the weakening time scales. The BAL variability amplitude correlates strongly with the BAL properties compared to the quasar properties. BALs with low W, high-velocity, shallow profiles, and low-velocity width tend to show more variability. When multiple BAL components are present a correlated variability is seen between low- and high-velocity components with the latter showing larger amplitude variations. We find an anti-correlation between the fractional variations in the continuum flux and W. While this suggests photoionization-induced variability, the scatter in continuum flux is much smaller than that of W.
description: 22 pages, accepted for publication in MNRAS
title: ÐÐ±ÐµÑÐ¿ÐµÑÐµÐ½Ð¸Ðµ Ð´Ð¸ÑÑÐ¸Ð¿Ð»Ð¸Ð½Ñ Ð¸ Ð·Ð°ÐºÐ¾Ð½Ð½Ð¾ÑÑÐ¸ Ð² ÑÑÐµÑÐµ Ð¸ÑÐ¿Ð¾Ð»Ð½Ð¸ÑÐµÐ»ÑÐ½Ð¾Ð¹ Ð²Ð»Ð°ÑÑÐ¸
title: Ð±Ð°ÐºÐ°Ð»Ð°Ð²ÑÑÐºÐ°Ñ ÑÐ°Ð±Ð¾ÑÐ°
titleType: Subtitle
Creators: name: ÐÐ¾ÑÐ¾Ð½Ð¸Ð½, ÐÐ³Ð¾Ñ
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·Ð°ÐºÐ¾Ð½Ð½Ð¾ÑÑÑ
Ð´Ð¸ÑÑÐ¸Ð¿Ð»Ð¸Ð½Ð°
Ð¸ÑÐ¿Ð¾Ð»Ð½Ð¸ÑÐµÐ»ÑÐ½ÑÐµ Ð¾ÑÐ³Ð°Ð½Ñ Ð²Ð»Ð°ÑÑÐ¸
ÐºÐ¾Ð½ÑÑÐ¾Ð»Ñ
legality
discipline
executive avthories
control

description: ÐÑÐ¿ÑÑÐºÐ½Ð°Ñ ÐºÐ²Ð°Ð»Ð¸ÑÐ¸ÐºÐ°ÑÐ¸Ð¾Ð½Ð½Ð°Ñ ÑÐ°Ð±Ð¾ÑÐ° Ð¿Ð¾ÑÐ²ÑÑÐµÐ½Ð° Ð¸ÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð¸Ñ Ð²Ð¾Ð¿ÑÐ¾ÑÐ¾Ð² Ð´Ð¸ÑÑÐ¸Ð¿Ð»Ð¸Ð½Ñ Ð¸ Ð·Ð°ÐºÐ¾Ð½Ð½Ð¾ÑÑÐ¸ Ð² ÑÑÐµÑÐµ Ð¸ÑÐ¿Ð¾Ð»Ð½Ð¸ÑÐµÐ»ÑÐ½Ð¾Ð¹ Ð²Ð»Ð°ÑÑÐ¸. Ð Ð°ÑÑÐ¼Ð°ÑÑÐ¸Ð²Ð°ÑÑÑÑ Ð¿Ð¾Ð½ÑÑÐ¸Ñ Â«Ð·Ð°ÐºÐ¾Ð½Ð½Ð¾ÑÑÑÂ», Â«Ð´Ð¸ÑÑÐ¸Ð¿Ð»Ð¸Ð½Ð°Â», Ð° ÑÐ°ÐºÐ¶Ðµ Ð¿ÑÐ¾Ð²Ð¾Ð´Ð¸ÑÑÑ ÑÑÐ°Ð²Ð½Ð¸ÑÐµÐ»ÑÐ½Ð¾-Ð¿ÑÐ°Ð²Ð¾Ð²Ð¾Ð¹ Ð°Ð½Ð°Ð»Ð¸Ð· ÑÐ¸ÑÑÐµÐ¼Ñ Ð¸ÑÐ¿Ð¾Ð»Ð½Ð¸ÑÐµÐ»ÑÐ½Ð¾Ð¹ Ð²Ð»Ð°ÑÑÐ¸ Ð² Ð Ð¾ÑÑÐ¸Ð¹ÑÐºÐ¾Ð¹ Ð¤ÐµÐ´ÐµÑÐ°ÑÐ¸Ð¸. Ð ÑÐ°Ð±Ð¾ÑÐµ Ð¾Ð¿ÑÐµÐ´ÐµÐ»ÐµÐ½Ñ Ð¾ÑÐ½Ð¾Ð²Ð½ÑÐµ Ð¿Ð¾Ð»Ð½Ð¾Ð¼Ð¾ÑÐ¸Ñ Ð¸ ÑÑÐ½ÐºÑÐ¸Ð¸ Ð¾ÑÐ³Ð°Ð½Ð¾Ð² Ð³Ð¾ÑÑÐ´Ð°ÑÑÑÐ²ÐµÐ½Ð½Ð¾Ð¹ Ð²Ð»Ð°ÑÑÐ¸ Ð¿ÑÐ¸ Ð¾ÑÑÑÐµÑÑÐ²Ð»ÐµÐ½Ð¸Ð¸ ÐºÐ¾Ð½ÑÑÐ¾Ð»Ñ Ð·Ð° Ð·Ð°ÐºÐ¾Ð½Ð½Ð¾ÑÑÑÑ Ð¸ Ð´Ð¸ÑÑÐ¸Ð¿Ð»Ð¸Ð½Ð¾Ð¹ Ð² ÑÑÐµÑÐµ Ð¸ÑÐ¿Ð¾Ð»Ð½Ð¸ÑÐµÐ»ÑÐ½Ð¾Ð¹ Ð²Ð»Ð°ÑÑÐ¸.
description: Final qualification work is devoted to a research of questions of discipline and legality in the sphere of executive power. The concepts "legality", "discipline" are considered, and also the comparative and legal analysis of system of executive power in the Russian Federation is carried out. In work the main powers and functions of public authorities at control of legality and discipline in the sphere of executive power are defined.
What's next after notebooks?
Creators: name: Morley, Alexander
Publisher: name: Zenodo
Year: 2019
Subjects: research
software
jupyter

description: Jane is a data scientist. Jane uses Jupyter notebooks as her working environment, and her presentation environment. These “computational essays” allow Jane to present her methods and her results to her colleagues at the same time. Jane is happy with this. But sometimes it’s difficult for Jane to share notebooks with her colleagues, and even harder for them to re-mix or re-use parts of the notebook, or to share their changes back to Jane. And sometimes Jane finds it hard to explain the flow of a particular notebook, or how different notebooks are tied together. There’s no provision for keeping things modular. First, I will discuss a few up-and-coming projects that are leveraging the power of new web technologies and faster browsers to solve all of fictional Jane’s problems, and more. Second, I will present a prototype for my own solution that is also web-based, and draws inspiration from some now-uncool graphical programming languages.
Witnessing the intracluster medium assembly at the cosmic noon in JKCS041
Creators: name: Andreon, S.
name: Romero, C.
name: Aussel, H.
name: Bhandarkar, T.
name: Devlin, M.
name: Dicker, S.
name: Ladjelate, B.
name: Lowe, I.
name: Mason, B.
name: Mroczkowski, T.
name: Raichoor, A.
name: Sarazin, C.
name: Trinchieri, G.
Publisher: name: arXiv
Year: 2023
Subjects: subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: In this work we study the intracluster medium of a galaxy cluster at the cosmic noon: JKCS041 at z=1.803. A 28h long Sunyaev-Zel'dovich (SZ) observation using MUSTANG-2 allows us to detect JKCS041, even if intrinsically extremely faint compared to other SZ-detected clusters. We found that the SZ peak is offset from the X-ray center by about 220 kpc in the direction of the brightest cluster galaxy, which we interpret as due to the cluster being observed just after first passage of a major merger. JKCS041 has a low central pressure and a low Compton Y compared to local clusters selected by their intracluster medium (ICM), likely because the cluster is still in the process of assembly but also in part because of a hard-to-quantify bias in current local ICM-selected samples. JKCS041 has a 0.5 dex fainter Y signal than another less massive z~1.8 cluster, exemplifying how much different weak-lensing mass and SZ mass can be at high redshift. The observations we present provide us with the measurement of the most distant resolved pressure profile of a galaxy cluster. Comparison with a library of plausibly descendants shows that JKCS041 pressure profile will likely increase by about 0.7 dex in the next 10 Gyr at all radii.
description: MNRAS, in press
Instabilities in dusty non-isothermal proto-planetary discs
Creators: name: Lehmann, Marius
name: Lin, Min-Kai
Publisher: name: arXiv
Year: 2023
Subjects: subject: Earth and Planetary Astrophysics (astro-ph.EP)
subject: FOS: Physical sciences

description: Protoplanetary discs (PPDs) can host a number of instabilities that may partake directly or indirectly in the process of planetesimal formation. These include the Vertical Shear Instability (VSI), Convective Overstability (COS), Streaming Instability (SI), and Dust Settling Instability (DSI), to name a few. Notably, the VSI and COS have mostly been studied in purely gaseous discs, while the SI and DSI have only been analyzed in isothermal discs. How these instabilities operate under more general conditions is therefore unclear. To this end, we devise a local model of a PPD describing a non-isothermal gas interacting with a single species of dust via drag forces. Using this, we find that dust drag sets minimum length scales below which the VSI and COS are suppressed. Similarly, we find that the SI can be suppressed on sufficiently small scales by the gas' radial buoyancy if it cools on roughly a dynamical timescale. We show that the DSI can be effectively stabilized by vertical buoyancy, except at special radial and vertical length scales. We also find novel instabilities unique to a dusty, non-isothermal gas. These result in a dusty analog of the COS that operates in slowly cooled discs, and a dusty version of the VSI that is strongly enhanced by dust settling. We briefly discuss the possible implications of our results on planetesimal formation.
description: 40 pages, 26 figures
Crises in NCP, Nepal in crises: The Iceberg Floats on the Bottom of the Sea
Creators: name: Sanjayprasad Paudel
Publisher: name: figshare
Year: 2021
Subjects: subject: 160801 Applied Sociology, Program Evaluation and Social Impact Assessment
subject: FOS: Sociology
subject: 160699 Political Science not elsewhere classified
subject: FOS: Political science

description: A few critiques define the present step of PM Oli as a “U” turn and regression in the way of Nepalese politics and prosperity that the people of Nepal have ever sought. In the general election in 2017 AD NCP has attained nearly two third of majority in the parliament in Nepalese political history after the election in 2015 B.S. when Nepali Congress had attained two third of majority.
Colossal magnetoresistance in an ultra-clean weakly interacting 2D Fermi liquid
Creators: name: Zhou, Xiaoqing
name: Piot, B. A.
name: Bonin, M.
name: Engel, L. W.
name: Sarma, S. Das
name: Gervais, G.
name: Pfeiffer, L. N.
name: West, K. W.
Publisher: name: arXiv
Year: 2010
Subjects: subject: Strongly Correlated Electrons (cond-mat.str-el)
subject: Mesoscale and Nanoscale Physics (cond-mat.mes-hall)
subject: FOS: Physical sciences

description: We report the observation of a new phenomenon of colossal magnetoresistance in a 40 nm wide GaAs quantum well in the presence of an external magnetic field applied parallel to the high-mobility 2D electron layer. In a strong magnetic field, the magnetoresistance is observed to increase by a factor of ~300 from 0 to 45T without the system undergoing any metal-insulator transition. We discuss how this colossal magnetoresistance effect cannot be attributed to the spin degree-of-freedom or localization physics, but most likely emanates from strong magneto-orbital coupling between the two-dimensional electron gas and the magnetic field. Our observation is consistent with a field-induced 2D-to-3D transition in the confined electronic system.
title: Ð£Ð¿ÑÐ°Ð²Ð»ÐµÐ½Ð¸Ðµ ÐºÐ°ÑÐµÑÑÐ²Ð¾Ð¼
title: ÑÑÐµÐ±Ð½Ð¾Ðµ Ð¿Ð¾ÑÐ¾Ð±Ð¸Ðµ
titleType: Subtitle
Creators: name: Ð§ÐµÑÐ½Ð¸ÐºÐ¾Ð²Ð°, ÐÐ½Ð½Ð°
name: ÐÑÐ¼Ð¸Ð½, ÐÐ¾ÑÐ¸Ñ
Publisher: name: ÐÐÐÐÐ¢ÐÐ¥-ÐÐ ÐÐ¡Ð¡
Year: 2021
Subjects: ÑÐºÐ¾Ð½Ð¾Ð¼Ð¸ÐºÐ°
ÑÐ¿ÑÐ°Ð²Ð»ÐµÐ½Ð¸Ðµ ÐºÐ°ÑÐµÑÑÐ²Ð¾Ð¼
ÑÑÐµÐ±Ð½Ð¸ÐºÐ¸ Ð¸ Ð¿Ð¾ÑÐ¾Ð±Ð¸Ñ Ð´Ð»Ñ Ð²ÑÐ·Ð¾Ð²

description: Ð¡Ð¾Ð´ÐµÑÐ¶Ð°Ð½Ð¸Ðµ Ð¿Ð¾ÑÐ¾Ð±Ð¸Ñ Ð¿Ð¾ÑÐ²ÑÑÐµÐ½Ð¾ ÑÐ°ÑÑÐ¼Ð¾ÑÑÐµÐ½Ð¸Ñ Ð²Ð¾Ð¿ÑÐ¾ÑÐ¾Ð², Ð½Ð°Ð¿ÑÐ°Ð²Ð»ÐµÐ½Ð½ÑÑ Ð½Ð° Ð¾ÐºÐ°Ð·Ð°Ð½Ð¸Ðµ Ð¼ÐµÑÐ¾Ð´Ð¸ÑÐµÑÐºÐ¾Ð¹ Ð¿Ð¾Ð¼Ð¾ÑÐ¸ ÑÑÑÐ´ÐµÐ½ÑÐ°Ð¼ Ð² Ð²ÑÐ¿Ð¾Ð»Ð½ÐµÐ½Ð¸Ð¸ Ð¿ÑÐ°ÐºÑÐ¸ÑÐµÑÐºÐ¸Ñ Ð·Ð°Ð´Ð°Ð½Ð¸Ð¹ Ð¿Ð¾ Ð´Ð¸ÑÑÐ¸Ð¿Ð»Ð¸Ð½Ðµ Â«Ð£Ð¿ÑÐ°Ð²Ð»ÐµÐ½Ð¸Ðµ ÐºÐ°ÑÐµÑÑÐ²Ð¾Ð¼Â», Ð½Ð° ÑÐ¾ÑÐ¼Ð¸ÑÐ¾Ð²Ð°Ð½Ð¸Ðµ ÐºÐ¾Ð¼Ð¿ÐµÑÐµÐ½ÑÐ¸Ð¹, Ð½ÐµÐ¾Ð±ÑÐ¾Ð´Ð¸Ð¼ÑÑ Ð´Ð»Ñ Ð°Ð½Ð°Ð»Ð¸Ð·Ð°, Ð¾ÑÐµÐ½ÐºÐ¸ Ð¸ ÑÐ¿ÑÐ°Ð²Ð»ÐµÐ½Ð¸Ñ ÐºÐ°ÑÐµÑÑÐ²Ð¾Ð¼ Ð½Ð° Ð¿ÑÐµÐ´Ð¿ÑÐ¸ÑÑÐ¸ÑÑ ÑÐ°Ð·Ð»Ð¸ÑÐ½ÑÑ Ð¾ÑÑÐ°ÑÐ»ÐµÐ¹ ÑÐºÐ¾Ð½Ð¾Ð¼Ð¸ÐºÐ¸. ÐÐ¾ÑÐ¾Ð±Ð¸Ðµ ÑÐ¾Ð´ÐµÑÐ¶Ð¸Ñ Ð¿ÑÐ°ÐºÑÐ¸ÑÐµÑÐºÐ¸Ðµ Ð·Ð°Ð´Ð°Ð½Ð¸Ñ Ð¸ ÑÐ¸ÑÑÐ°ÑÐ¸Ð¾Ð½Ð½ÑÐµ Ð·Ð°Ð´Ð°ÑÐ¸, ÑÑÐ¾ Ð¾Ð±ÑÑÐ»Ð¾Ð²Ð»ÐµÐ½Ð¾ Ð¾ÑÐ½Ð¾Ð²Ð½ÑÐ¼Ð¸ ÑÐ°Ð·Ð´ÐµÐ»Ð°Ð¼Ð¸ Ð´Ð¸ÑÑÐ¸Ð¿Ð»Ð¸Ð½Ñ Â«Ð£Ð¿ÑÐ°Ð²Ð»ÐµÐ½Ð¸Ðµ ÐºÐ°ÑÐµÑÑÐ²Ð¾Ð¼Â», ÐºÐ¾ÑÐ¾ÑÑÐµ Ð¿Ð¾Ð·Ð²Ð¾Ð»ÑÑ ÑÑÐ¿ÐµÑÐ½Ð¾ Ð¾ÑÐ²Ð¾Ð¸ÑÑ Ð¼Ð½Ð¾Ð³Ð¾Ð¾Ð±ÑÐ°Ð·Ð¸Ðµ Ð°ÑÐ¿ÐµÐºÑÐ¾Ð² Ð´Ð¸ÑÑÐ¸Ð¿Ð»Ð¸Ð½Ñ Ð¿ÑÐ¸Ð¼ÐµÐ½Ð¸ÑÐµÐ»ÑÐ½Ð¾ Ðº ÑÐ°Ð·Ð½ÑÐ¼ Ð¾Ð±ÑÐµÐºÑÐ°Ð¼ â ÑÐ¾Ð²Ð°ÑÐ°Ð¼, ÑÑÐ»ÑÐ³Ð°Ð¼, Ð¿ÑÐ¾ÑÐµÑÑÐ°Ð¼. ÐÑÐµÐ´Ð½Ð°Ð·Ð½Ð°ÑÐµÐ½Ð¾ Ð´Ð»Ñ ÑÑÑÐ´ÐµÐ½ÑÐ¾Ð² Ð½Ð°Ð¿ÑÐ°Ð²Ð»ÐµÐ½Ð¸Ð¹ Ð¸ ÑÐ¿ÐµÑÐ¸Ð°Ð»ÑÐ½Ð¾ÑÑÐµÐ¹ ÑÐ¾ÑÐ³Ð¾Ð²Ð¾-ÑÐºÐ¾Ð½Ð¾Ð¼Ð¸ÑÐµÑÐºÐ¾Ð¹ Ð¿Ð¾Ð»Ð¸Ð³ÑÑÐ¿Ð¿Ñ Ð¾ÑÐ½Ð¾Ð¹, Ð¾ÑÐ½Ð¾-Ð·Ð°Ð¾ÑÐ½Ð¾Ð¹ Ð¸ Ð·Ð°Ð¾ÑÐ½Ð¾Ð¹ ÑÐ¾ÑÐ¼ Ð¾Ð±ÑÑÐµÐ½Ð¸Ñ.
Instrumento de Entrevista fundamentado nos 4 princípios de conservação da Teoria de Myra Levine
Creators: name: Quintans Cundines Pacheco, Patrícia
Publisher: name: Zenodo
Year: 2024

description: Instrumento de Entrevista fundamentado nos 4 princípios de conservação da Teoria de Myra Levine. Este instrumento poderá ser aplicado para identificar as repercussões na saúde da mulher mãe de criança e adolescente com câncer.
The Long and the Short of It: The Benefits and Leverage of Ultraviolet-Radio Galaxy Fitting
Creators: name: Thorne, Jessica E.
name: Robotham, Aaron S. G.
name: Bellstedt, Sabine
name: Davies, Luke J. M.
Publisher: name: arXiv
Year: 2023
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: Traditionally, the far ultraviolet (FUV) to far-infrared (FIR) and radio spectral energy distributions (SEDs) of galaxies have been considered separately despite the common physical process shaping them. In this work, we explore the utility of simultaneously fitting FUV-radio SEDs using an extended version of the ProSpect SED fitting code considering contributions from both free-free and synchrotron emission. We use a small sample of galaxies from the Deep Extragalactic VIsible Legacy Survey (DEVILS) and the Key Insights on Nearby Galaxies: a Far-Infrared Survey with Herschel (KINGFISH) where high-quality and robust FUV-radio data are available to provide an ideal sample for testing a radio extension of ProSpect. As the parameterisation of the radio extension links the radio continuum to the FIR emission, we explore the benefit of using radio continuum measurements as a constraint on the energy balance between dust attenuation and emission. We find that for situations where MIR-FIR photometry is unavailable, including a 1.4 GHz continuum measurement allows for improved accuracy in recovered star formation rates and dust luminosities of galaxies reducing the median uncertainty by 0.1 and 0.2 dex respectively. We also demonstrate that incorporating 3 and 10 GHz measurements allows for further constraint on the energy balance and therefore the star formation rate and dust luminosity. This demonstrates the advantage of extending FUV-FIR SED fitting techniques to radio frequencies, especially as we move into an era where FIR surveys will remain limited and radio data become abundant (i.e. with the SKA and precursors).
description: Accepted for publication in MNRAS
Effective permittivity of mixtures of anisotropic particles
Creators: name: Sushko, M. Ya.
Publisher: name: arXiv
Year: 2009
Subjects: subject: Materials Science (cond-mat.mtrl-sci)
subject: Soft Condensed Matter (cond-mat.soft)
subject: FOS: Physical sciences

description: We use a new approach to derive dielectric mixing rules for macroscopically homogeneous and isotropic multicomponent mixtures of anisotropic inhomogeneous dielectric particles. Two factors of anisotropy are taken into account, the shape of the particles and anisotropy of the dielectric parameters of the particles' substances. Our approach is based upon the notion of macroscopic compact groups of particles and the procedure of averaging of the fields over volumes much greater than the typical scales of these groups. It enables us to effectively sum up the contributions from multiple interparticle reemission and short-range correlation effects, represented by all terms in the infinite iterative series for the electric field strength and induction. The expression for the effective permittivity can be given the form of the Lorentz-Lorenz type, which allows us to determine the effective polarizabilities of the particles in the mixture. These polarizabilities are found as integrals over the regions occupied by the particles and taken of explicit functions of the principal components of the permittivity tensors of the particles' substances and the permittivity of the host medium. The case of a mixture of particles of the ellipsoidal shape is considered in detail to exemplify the use of general formulas. As another example, Bruggeman-type formulas are derived under pertinent model assumptions. The ranges of validity of the results obtained are discussed as well.
description: 9 pages, 4 figures
title: Ð¡ÑÐ°ÑÐ¸ÑÑÐ¸ÐºÐ°. ÐÐµÑÐ¾Ð´Ñ Ð°Ð½Ð°Ð»Ð¸Ð·Ð° Ð¿ÑÐ¾Ð±Ð»ÐµÐ¼ Ð¼Ð¸ÑÐ¾Ð²Ð¾Ð¹ ÑÐºÐ¾Ð½Ð¾Ð¼Ð¸ÐºÐ¸
title: ÑÑÐµÐ±Ð½Ð¾Ðµ Ð¿Ð¾ÑÐ¾Ð±Ð¸Ðµ
titleType: Subtitle
Creators: name: ÐÐ½ÑÐ¸Ð¿Ð¾Ð², Ð¡ÐµÑÐ³ÐµÐ¹
Publisher: name: ÐÐ·Ð´-Ð²Ð¾ ÐÐ¾Ð»Ð¸ÑÐµÑÐ½. ÑÐ½-ÑÐ°
Year: 2012
Subjects: ÐÑÑÐ¸ÑÐ»Ð¸ÑÐµÐ»ÑÐ½ÑÐµ Ð¼Ð°ÑÐ¸Ð½Ñ ÑÐ»ÐµÐºÑÑÐ¾Ð½Ð½ÑÐµ
Ð¡ÑÐ°ÑÐ¸ÑÑÐ¸ÑÐµÑÐºÐ¸Ð¹ Ð°Ð½Ð°Ð»Ð¸Ð·
ÑÐºÐ¾Ð½Ð¾Ð¼Ð¸ÑÐµÑÐºÐ°Ñ ÑÑÐ°ÑÐ¸ÑÑÐ¸ÐºÐ°
Ð¼Ð¸ÑÐ¾Ð²Ð°Ñ ÑÐºÐ¾Ð½Ð¾Ð¼Ð¸ÐºÐ°
ÑÑÐµÐ±Ð½Ð¸ÐºÐ¸ Ð¸ Ð¿Ð¾ÑÐ¾Ð±Ð¸Ñ Ð´Ð»Ñ Ð²ÑÐ·Ð¾Ð²

description: ÐÑÐµÐ´ÑÑÐ°Ð²Ð»ÐµÐ½Ð¾ ÑÐ¸ÑÑÐµÐ¼Ð°ÑÐ¸Ð·Ð¸ÑÐ¾Ð²Ð°Ð½Ð½Ð¾Ðµ Ð¸Ð·Ð»Ð¾Ð¶ÐµÐ½Ð¸Ðµ Ð·Ð°Ð´Ð°Ñ ÑÑÐ°ÑÐ¸ÑÑÐ¸ÑÐµÑÐºÐ¾Ð¹ Ð½Ð°ÑÐºÐ¸, Ð°Ð½Ð°Ð»Ð¸Ð· Ð¿ÑÐ¾Ð±Ð»ÐµÐ¼ Ð¼Ð¸ÑÐ¾Ð²Ð¾Ð¹ ÑÐºÐ¾Ð½Ð¾Ð¼Ð¸ÐºÐ¸ Ñ Ð¸ÑÐ¿Ð¾Ð»ÑÐ·Ð¾Ð²Ð°Ð½Ð¸ÐµÐ¼ ÑÑÐ°ÑÐ¸ÑÑÐ¸ÑÐµÑÐºÐ¸Ñ Ð¼Ð¾Ð´ÐµÐ»ÐµÐ¹ Ð¸ Ð¼ÐµÑÐ¾Ð´Ð¾Ð².
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ÐÑÐµÐ´Ð½Ð°Ð·Ð½Ð°ÑÐµÐ½Ð¾ Ð´Ð»Ñ ÑÑÑÐ´ÐµÐ½ÑÐ¾Ð², Ð¾Ð±ÑÑÐ°ÑÑÐ¸ÑÑÑ Ð¿Ð¾ Ð½Ð°Ð¿ÑÐ°Ð²Ð»ÐµÐ½Ð¸Ñ Â«Ð­ÐºÐ¾Ð½Ð¾Ð¼Ð¸ÐºÐ°Â» Ð¿Ð¾ ÑÐ¿ÐµÑÐ¸Ð°Ð»ÑÐ½Ð¾ÑÑÐ¸ Â«ÐÐ¸ÑÐ¾Ð²Ð°Ñ ÑÐºÐ¾Ð½Ð¾Ð¼Ð¸ÐºÐ°Â» Ð¸ Ð´ÑÑÐ³Ð¸Ð¼ ÑÐºÐ¾Ð½Ð¾Ð¼Ð¸ÑÐµÑÐºÐ¸Ð¼ ÑÐ¿ÐµÑÐ¸Ð°Ð»ÑÐ½Ð¾ÑÑÑÐ¼, Ð´Ð»Ñ Ð¿ÑÐµÐ¿Ð¾Ð´Ð°Ð²Ð°ÑÐµÐ»ÐµÐ¹, Ð° ÑÐ°ÐºÐ¶Ðµ Ð´Ð»Ñ ÑÐ¸ÑÐ¾ÐºÐ¾Ð³Ð¾ ÐºÑÑÐ³Ð° ÑÐ¸ÑÐ°ÑÐµÐ»ÐµÐ¹, Ð¸Ð½ÑÐµÑÐµÑÑÑÑÐ¸ÑÑÑ Ð´Ð°Ð½Ð½Ð¾Ð¹ ÑÐµÐ¼Ð°ÑÐ¸ÐºÐ¾Ð¹.
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°.
Synchrotron intensity plots from a relativistic stratified jet
Creators: name: Frolova, V. A.
name: Nokhrina, E. E.
name: Pashchenko, I. N.
Publisher: name: arXiv
Year: 2023
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: We examine the effect of a jet transversal structure from magnetohydrodynamic semi-analytical modelling on the total intensity profiles of relativistic jets from active galactic nuclei. In order to determine the conditions for forming double- and triple-peaked transverse intensity profiles, we calculate the radiative transfer for synchrotron emission with self-absorption from the jets described by the models with a constant angular velocity and with a total electric current closed inside a jet. We show that double-peaked profiles appear either in the models with high maximal Lorentz factors or in optically thick conditions. We show that triple-peaked profiles in radio galaxies constrain the fraction of the emitting particles in a jet. We introduce the possible conditions for triple-peaked profiles under the assumptions that nonthermal electrons are preferably located at the jet edges or are distributed according to Ohmic heating.
description: 22 pages, 11 figures, accepted by MNRAS
title: ÐÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð¸Ðµ Ð²Ð¾Ð·Ð¼Ð¾Ð¶Ð½Ð¾ÑÑÐµÐ¹ ÑÐ°ÑÑÐµÑÐ° Ð±Ð¸Ð¾Ð¼ÐµÑ Ð°Ð½Ð¸ÑÐµÑÐºÐ¸Ñ ÑÐ¸ÑÑÐµÐ¼ Ð¼ÐµÑÐ¾Ð´Ð¾Ð¼ ÐºÐ¾Ð½ÐµÑÐ½ÑÑ ÑÐ»ÐµÐ¼ÐµÐ½ÑÐ¾Ð²
title: Ð±Ð°ÐºÐ°Ð»Ð°Ð²ÑÑÐºÐ°Ñ ÑÐ°Ð±Ð¾ÑÐ°
titleType: Subtitle
Creators: name: Ð¢Ð¸ÑÐ¾Ð², 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: 2017
Subjects: Ð±Ð¸Ð¾Ð¼ÐµÑ Ð°Ð½Ð¸ÐºÐ°
Ð¼ÐµÑÐ¾Ð´ ÐºÐ¾Ð½ÐµÑÐ½ÑÑ ÑÐ»ÐµÐ¼ÐµÐ½ÑÐ¾Ð²
Ð¼Ð°ÑÐµÐ¼Ð°ÑÐ¸ÑÐµÑÐºÐ¾Ðµ Ð¼Ð¾Ð´ÐµÐ»Ð¸ÑÐ¾Ð²Ð°Ð½Ð¸Ðµ

description: ÐÑÐµÐ´Ð¼ÐµÑÐ¾Ð¼ Ð¸ÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð¸Ñ Ð´Ð¸Ð¿Ð»Ð¾Ð¼Ð½Ð¾Ð³Ð¾ Ð¿ÑÐ¾ÐµÐºÑÐ° ÑÐ²Ð»ÑÐµÑÑÑ Ð¼ÐµÑÐ¾Ð´ ÐºÐ¾Ð½ÐµÑÐ½ÑÑ ÑÐ»ÐµÐ¼ÐµÐ½ÑÐ¾Ð². ÐÐ¸Ð¿Ð»Ð¾Ð¼Ð½ÑÐ¹ Ð¿ÑÐ¾ÐµÐºÑ ÑÐ¾ÑÑÐ¾Ð¸Ñ Ð¸Ð· Ð²Ð²ÐµÐ´ÐµÐ½Ð¸Ñ, ÑÑÐµÑ ÑÐ°Ð·Ð´ÐµÐ»Ð¾Ð² Ð¸ Ð·Ð°ÐºÐ»ÑÑÐµÐ½Ð¸Ñ. ÐÐ²ÐµÐ´ÐµÐ½Ð¸Ðµ Ð¾Ð±Ð¾ÑÐ½Ð¾Ð²ÑÐ²Ð°ÐµÑ Ð°ÐºÑÑÐ°Ð»ÑÐ½Ð¾ÑÑÑ Ð²ÑÐ±ÑÐ°Ð½Ð½Ð¾Ð¹ ÑÐµÐ¼Ñ, ÑÐ¾ÑÐ¼ÑÐ»Ð¸ÑÑÐµÑ ÑÐµÐ»Ñ Ð¸ÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð¸Ñ, ÑÐºÐ°Ð·ÑÐ²Ð°ÐµÑ Ð¾Ð±ÑÐµÐºÑ Ð¸ Ð¿ÑÐµÐ´Ð¼ÐµÑ Ð¸ÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð¸Ñ. ÐÐµÑÐ²ÑÐ¹ ÑÐ°Ð·Ð´ÐµÐ» Ð´Ð°ÐµÑ ÑÐ°ÑÐ°ÐºÑÐµÑÐ¸ÑÑÐ¸ÐºÑ Ð¼ÐµÑÐ¾Ð´Ð¾Ð² Ð¿Ð¾ÑÑÑÐ¾ÐµÐ½Ð¸Ñ Ð¼Ð¾Ð´ÐµÐ»ÐµÐ¹ Ð¸ Ð¾Ð¿Ð¸ÑÑÐ²Ð°ÐµÑ ÑÐ¿Ð¾ÑÐ¾Ð±Ñ Ð¸Ñ ÑÐµÐ°Ð»Ð¸Ð·Ð°ÑÐ¸Ð¸ Ð² ÑÐ¾Ð²ÑÐµÐ¼ÐµÐ½Ð½Ð¾Ð¹ Ð½Ð°ÑÑÐ½Ð¾-Ð¿ÑÐ¾ÐµÐºÑÐ½Ð¾Ð¹ Ð´ÐµÑÑÐµÐ»ÑÐ½Ð¾ÑÑÐ¸ Ñ Ð¿ÑÐ¸Ð¼ÐµÐ½ÐµÐ½Ð¸ÐµÐ¼ Ð²ÑÑÐ¸ÑÐ»Ð¸ÑÐµÐ»ÑÐ½Ð¾Ð¹ ÑÐµÑÐ½Ð¸ÐºÐ¸. ÐÑÐ¾ÑÐ¾Ð¹ ÑÐ°Ð·Ð´ÐµÐ» Ð¿Ð¾ÑÐ²ÑÑÐµÐ½ Ð¸ÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð¸Ñ ÑÐµÐ¾ÑÐµÑÐ¸ÑÐµÑÐºÐ¸Ñ Ð²Ð¾Ð¿ÑÐ¾ÑÐ¾Ð². Ð Ð½ÐµÐ¼ ÑÐ°ÑÐºÑÑÐ²Ð°ÑÑÑÑ Ð¿Ð¾Ð½ÑÑÐ¸Ðµ Ð¸ ÑÑÑÐ½Ð¾ÑÑÑ ÑÐ¾Ð²ÑÐµÐ¼ÐµÐ½Ð½ÑÑ ÑÐ¿Ð¾ÑÐ¾Ð±Ð¾Ð² Ð¿Ð¾ÑÑÑÐ¾ÐµÐ½Ð¸Ñ Ð¼Ð°ÑÐµÐ¼Ð°ÑÐ¸ÑÐµÑÐºÐ¸Ñ Ð¼Ð¾Ð´ÐµÐ»ÐµÐ¹ Ð¼ÐµÑÐ°Ð½Ð¸ÑÐµÑÐºÐ¸Ñ ÑÐ¸ÑÑÐµÐ¼ Ñ Ð¸ÑÐ¿Ð¾Ð»ÑÐ·Ð¾Ð²Ð°Ð½Ð¸ÐµÐ¼ Ð¼ÐµÑÐ¾Ð´Ð° ÐºÐ¾Ð½ÐµÑÐ½ÑÑ ÑÐ»ÐµÐ¼ÐµÐ½ÑÐ¾Ð². Ð¢ÑÐµÑÐ¸Ð¹ ÑÐ°Ð·Ð´ÐµÐ» Ð´Ð°ÐµÑ Ð¾Ð¿Ð¸ÑÐ°Ð½Ð¸Ðµ Ð¾Ð±ÑÐµÐ³Ð¾ ÑÐ»ÑÑÐ°Ñ Ð¸ÑÐ¿Ð¾Ð»ÑÐ·Ð¾Ð²Ð°Ð½Ð¸Ñ Ð¼ÐµÑÐ¾Ð´Ð° ÐºÐ¾Ð½ÐµÑÐ½ÑÑ ÑÐ»ÐµÐ¼ÐµÐ½ÑÐ¾Ð² Ð¸ Ð¾Ð¿Ð¸ÑÑÐ²Ð°ÐµÑ ÐµÐ³Ð¾ Ð¿ÑÐµÐ¸Ð¼ÑÑÐµÑÑÐ²Ð° Ð¿ÐµÑÐµÐ´ Ð¾ÑÑÐ°Ð»ÑÐ½ÑÐ¼Ð¸ ÑÐ¸ÑÐ»ÐµÐ½Ð½ÑÐ¼Ð¸ Ð¼ÐµÑÐ¾Ð´Ð°Ð¼Ð¸. Ð§ÐµÑÐ²ÐµÑÑÑÐ¹ ÑÐ°Ð·Ð´ÐµÐ» Ð¸ÑÑÐ»ÐµÐ´ÑÐµÑ Ð¿ÑÐ°ÐºÑÐ¸ÐºÑ Ð¸ Ð²Ð¾Ð·Ð¼Ð¾Ð¶Ð½Ð¾ÑÑÐ¸ Ð¿ÑÐ¸Ð¼ÐµÐ½ÐµÐ½Ð¸Ñ Ð¼ÐµÑÐ¾Ð´Ð° ÐºÐ¾Ð½ÐµÑÐ½ÑÑ ÑÐ»ÐµÐ¼ÐµÐ½ÑÐ¾Ð² Ð² Ð±Ð¸Ð¾Ð¼ÐµÑÐ°Ð½Ð¸ÐºÐµ. ÐÐ°ÐºÐ»ÑÑÐµÐ½Ð¸Ðµ ÑÐ¾Ð´ÐµÑÐ¶Ð¸Ñ Ð¾ÑÐ½Ð¾Ð²Ð½ÑÐµ Ð²ÑÐ²Ð¾Ð´Ñ Ð¿Ð¾ Ð¿ÑÐ¾Ð´ÐµÐ»Ð°Ð½Ð½Ð¾Ð¹ ÑÐ°Ð±Ð¾ÑÐµ.
On the Cauchy Problem for the Korteweg-de Vries Equation with Steplike Finite-Gap Initial Data I. Schwartz-Type Perturbations
Creators: name: Egorova, Iryna
name: Grunert, Katrin
name: Teschl, Gerald
Publisher: name: arXiv
Year: 2008
Subjects: subject: Exactly Solvable and Integrable Systems (nlin.SI)
subject: Mathematical Physics (math-ph)
subject: Analysis of PDEs (math.AP)
subject: FOS: Physical sciences
subject: FOS: Mathematics

description: We solve the Cauchy problem for the Korteweg-de Vries equation with initial conditions which are steplike Schwartz-type perturbations of finite-gap potentials under the assumption that the respective spectral bands either coincide or are disjoint.
description: 29 pages
M92 (NGC~6341) Is a Metal-Complex Globular Cluster with an Atypical Primordial Population
Creators: name: Lee, Jae-Woo
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: We present a multiple stellar population study of the metal-poor globular cluster (GC) M92 (NGC 6341), which is long known for the substantial metallicity dispersion, using our own photometric system. We find two groups with slightly different mean metallicities, the metal-poor (MP) stars with [Fe/H] = $-$2.412$\pm$0.03, while the metal-rich (MR) ones with $-$2.282$\pm$0.002. The MP constitutes about 23\% of the total mass with a more central concentration. Our populational tagging based on the [C/Fe] and [N/Fe] provides the mean n(P):n(I):n(E) = 32.2:31.6:36.2 ($\pm$2.4), where P, I, and E denote the primordial, intermediate, and extreme populations, respectively. Our populational number ratio is consistent with those of others. However, the MP has a significantly different populational number ratio than the mean value, and the domination of the primordial population in the MP is consistent with observations of Galactic GCs that less massive GCs contain larger fractions of the primordial population. Structural and constituent differences between the MP and MR may indicate that M92 is a merger remnant in a dwarf galaxy environment, consistent with recent suggestions that M92 is a GC in a dwarf galaxy or a remnant nucleus of the progenitor galaxy. Discrepancy between our method and those widely used for the HST photometry exists in the primordial population. Significant magnesium and oxygen depletions of $-$0.8 and $-$0.3 dex, respectively, and helium enhancement of $ΔY$ $\gtrsim$ 0.03 are required to explain the presence of this abnormal primordial group. No clear explanation is available with limited information of detailed elemental abundances.
description: Accepted for publication to the Astrophysical Journal Letters
Anderson Localization of Classical Waves in Weakly Scattering Metamaterials
Creators: name: Asatrian, Ara A.
name: Gredeskul, Sergey A.
name: Botten, Lindsay C.
name: Byrne, Michael A.
name: Freilikher, Valentin D.
name: Shadrivov, Ilya V.
name: McPhedran, Ross C.
name: Kivshar, Yuri S.
Publisher: name: arXiv
Year: 2009
Subjects: subject: Disordered Systems and Neural Networks (cond-mat.dis-nn)
subject: Mesoscale and Nanoscale Physics (cond-mat.mes-hall)
subject: FOS: Physical sciences

description: We study the propagation and localization of classical waves in one-dimensional disordered structures composed of alternating layers of left- and right-handed materials (mixed stacks) and compare them to the structures composed of different layers of the same material (homogeneous stacks). For weakly scattering layers, we have developed an effective analytical approach and have calculated the transmission length within a wide region of the input parameters. When both refractive index and layer thickness of a mixed stack are random, the transmission length in the long-wave range of the localized regime exhibits a quadratic power wavelength dependence with the coefficients different for mixed and homogeneous stacks. Moreover, the transmission length of a mixed stack differs from reciprocal of the Lyapunov exponent of the corresponding infinite stack. In both the ballistic regime of a mixed stack and in the near long-wave region of a homogeneous stack, the transmission length of a realization is a strongly fluctuating quantity. In the far long-wave part of the ballistic region, the homogeneous stack becomes effectively uniform and the transmission length fluctuations are weaker. The crossover region from the localization to the ballistic regime is relatively narrow for both mixed and homogeneous stacks. In mixed stacks with only refractive-index disorder, Anderson localization at long wavelengths is substantially suppressed, with the localization length growing with the wavelength much faster than for homogeneous stacks. The crossover region becomes essentially wider and transmission resonances appear only in much longer stacks. All theoretical predictions are in an excellent agreement with the results of numerical simulations.
description: 19 pages, 16 figures, submitted to PRB
The Jeans Mechanism and Bulk-Viscosity Effects
Creators: name: Carlevaro, Nakia
name: Montani, Giovanni
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: In this paper we study the gravitational instability in presence of viscosity. In particular, the standard Jeans Mechanism is analyzed taking into account bulk-viscosity effects in the first-order Newtonian dynamics. We show how the perturbation evolution is damped by dissipative processes and the top-down fragmentation mechanism is suppressed for strong viscous effects. The critical value of the Jeans Mass remains unchanged also in presence of bulk viscosity.
description: Proceedings of The 3rd Stueckelberg Workshop on Relativistic Field Theories
Mildly Relativistic Motion in the Radio Quiet Quasar PG 1351+640
Creators: name: Wang, Ailing
name: An, Tao
name: Guo, Shaoguang
name: Ho, Luis C.
name: Baan, Willem A.
name: Braun, Robert
name: Chen, Sina
name: Cheng, Xiaopeng
name: Hartley, Philippa
name: Yang, Jun
name: Zhang, Yingkang
Publisher: name: arXiv
Year: 2023
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: Measuring the proper motion of the emission component in radio-quiet quasars (RQQs) could help to distinguish between the origins of the radio emission and to understand whether the jet production mechanism is the same in radio-loud quasars (RLQs) and RQQs. PG 1351+640 is one of the few RQQs suitable for proper motion studies: it has two compact components on milli-arcsecond scales, a flat-spectrum core and a steep-spectrum jet; both components are >2 mJy at 5 GHz and are well suited for Very Long Baseline Array (VLBA) observations. We compare recent VLBA observations with that made seventeen years ago and find no significant change in the core-jet separation between 2005 and 2015 (a proper motion of 0.003 mas yr-1). However, the core-jet separation increased significantly between 2015 and 2022, inferring a jet proper motion velocity of 0.063 mas yr-1, which corresponds to an apparent transverse velocity of 0.37c. The result suggests that the jet of the RQQ PG 1351+640 is mildly relativistic and oriented at a relatively small viewing angle.
description: The article has been published by Oxford University Press: https://academic.oup.com/mnrasl/advance-article-abstract/doi/10.1093/mnrasl/slad051/7146829?utm_source=advanceaccess&utm_campaign=mnrasl&utm_medium=email
Evolution of two stellar populations in globular clusters II. Effects of primordial gas expulsion
Creators: name: Decressin, T.
name: Baumgardt, H.
name: Charbonnel, C.
name: Kroupa, P.
Publisher: name: arXiv
Year: 2010
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences

description: We investigate the early evolution of two distinct populations of low-mass stars in globular clusters under the influence of primordial gas expulsion driven by supernovae to study if this process can increase the fraction of second generation stars at the level required by observations. We analyse N-body models that take into account the effect of primordial gas expulsion. We divide the stars into two populations which mimic the chemical and dynamical properties of stars in globular clusters so that second generation stars start with a more centrally concentrated distribution. The main effect of gas expulsion is to eject preferentially first generation stars while second generation stars remain bound to the cluster. In the most favourable cases second generation stars can account for 60% of the bound stars we see today. We also find that at the end of the gas expulsion phase, the radial distribution of the two populations is still different, so that long-term evolution will further increase the fraction of second generation stars. The large fraction of chemically anomalous stars is readily explainable as a second generation of stars formed out of the slow winds of rapidly rotating massive stars if globular clusters suffer explosive residual gas expulsion for a star formation efficiency of about 0.33.
description: 11 pages, accepted for publication in A&A
Revealing infrared populations of nearby galaxies using the Spitzer Space Telescope
Creators: name: Matsuura, Mikako
Publisher: name: arXiv
Year: 2009
Subjects: subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences

description: Due to their brightness in infrared, asymptotic giant branch (AGB) stars are in important evolutionary stage to be understood at this wavelength. In particular, in next decades, when the infrared optimised telescopes, such as the JWST and the ELT are in operation, it will be essential to include the AGB phase more precisely into the population synthesis models. However, the AGB phase is still one of the remaining major problems in the stellar evolution. This is because the AGB stellar evolution is strongly affected by the mass-loss process from the stars. It is important to describe mass loss more accurately so as to incorporate it into stellar evolutionary models. Recent observations using the Spitzer Space Telescope (SST) enabled us to make a significant progress in understanding the mass loss from AGB stars. Moreover, the SST large surveys contributed to our understanding of the role of AGB stars in chemical enrichment process in galaxies. Here we present the summary of our recent progress.
description: 4 pages, 2 figures, 1 table; IAU S262 proceedings
Evolution of the X-ray Luminosity in Young HII Galaxies
Creators: name: González, D. Rosa
name: Terlevich, E.
name: Bailón, E. Jiménez
name: Terlevich, R.
name: Ranalli, P.
name: Comastri, A.
name: Laird, E.
name: Nandra, K.
Publisher: name: arXiv
Year: 2009
Subjects: subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: FOS: Physical sciences

description: In an effort to understand the correlation between X-ray emission and present star formation rate (SFR), we obtained XMM-Newton data to estimate the X-ray luminosities of a sample of actively starforming HII galaxies. The obtained X-ray luminosities are compared to other well known tracers of star formation activity such as the far infrared and the ultraviolet luminosities. We also compare the obtained results with empirical laws from the literature and with recently published analysis applying synthesis models. We use the time delay between the formation of the stellar cluster and that of the first X-ray binaries, in order to put limits on the age of a given stellar burst. We conclude that the generation of soft X-rays, as well as the Ha or infrared luminosities is instantaneous. The relation between the observed radio and hard X-ray luminosities, on the other hand, points to the existence of a time delay between the formation of the stellar cluster and the explosion of the first massive stars and the consequent formation of supernova remnants and high mass X-ray binaries (HMXB) which originate the radio and hard X-ray fluxes respectively. When comparing hard X-rays with a star formation indicator that traces the first million years of evolution (e.g. Ha luminosities) we found a deficit in the expected X-ray luminosity. This deficit is not found when the X-ray luminosities are compared with infrared luminosities, a star formation tracer that represents an average over the last 10^8 years. The results support the hypothesis that hard X-rays are originated in X-ray binaries which, as supernova remnants, have a formation time delay of a few mega years after the starforming burst.
description: Accepted by MNRAS
A implementação de um sistema CRIS na Universidade Católica Portuguesa
Creators: name: Marçal, Bruno
name: Folque, Ana
name: Dias, João
name: Catanho, Cláudia
name: Perdigão, Maria
Publisher: name: Zenodo
Year: 2021

description: Apresentação realizada na sessão O meu Póster num minuto da 12ª Conferência Luso-Brasileira de Ciência Aberta, formato híbrido, de 13 a 15 de outubro de 2021.
The role of the drag force in the gravitational stability of dusty planet-forming disc -- II. Numerical simulations
Creators: name: Longarini, Cristiano
name: Armitage, Philip J.
name: Lodato, Giuseppe
name: Price, Daniel J.
name: Ceppi, Simone
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: Young protostellar discs are likely to be both self-gravitating, and to support grain growth to sizes where the particles decoupled from the gas. This combination could lead to short-wavelength fragmentation of the solid component in otherwise non-fragmenting gas discs, forming Earth-mass solid cores during the Class 0/I stages of Young Stellar Object evolution. We use three-dimensional smoothed particle hydrodynamics simulations of two-fluid discs, in the regime where the Stokes number of the particles St>1, to study how the formation of solid clumps depends on the disc-to-star mass ratio, the strength of gravitational instability, and the Stokes number. Gravitational instability of the simulated discs is sustained by local cooling. We find that the ability of the spiral structures to concentrate solids increases with the cooling time, and decreases with the Stokes number, while the relative dynamical temperature between gas and dust of the particles decreases with the cooling time and the disc-to-star mass ratio, and increases with the Stokes number. Dust collapse occurs in a subset of high disc mass simulations, yielding clumps whose mass is close to linear theory estimates, namely 1-10 Earth masses. Our results suggest that if planet formation occurs via this mechanism, the best conditions correspond to near the end of the self-gravitating phase, when the cooling time is long and the Stokes number close to unity.
description: Accepted for publication in MNRAS, 20 pages
Peering into the central region of a nano-quasar: XMM-Newton and Chandra views of the CH Cyg Symbiotic System
Creators: name: Toalá, J. A.
name: González-Martín, O.
name: Karovska, M.
name: Montez, R.
name: Botello, M. K.
name: Sabin, L.
Publisher: name: arXiv
Year: 2023
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: We present the analysis of archival XMM-Newton and Chandra observations of CH Cyg, one of the most studied symbiotic stars (SySts). The combination of the high-resolution XMM-Newton RGS and Chandra HETG X-ray spectra allowed us to obtain reliable estimates of the chemical abundances and to corroborate the presence of multi-temperature X-ray-emitting gas. Spectral fitting of the medium-resolution XMM-Newton MOS (MOS1+MOS2) spectrum required the use of an additional component not seen in previous studies in order to fit the 2.0-4.0 keV energy range. Detailed spectral modelling of the XMM-Newton MOS data suggests the presence of a reflection component, very similar to that found in active galactic nuclei. The reflection component is very likely produced by an ionised disk (the accretion disk around the white dwarf) and naturally explains the presence of the fluorescent Fe emission line at 6.4 keV while also contributing to the soft and medium energy ranges. The variability of the global X-ray properties of CH Cyg are discussed as well as the variation of the three Fe lines around the 6-7 keV energy range. We conclude that reflection components are needed to model the hard X-ray emission and may be present in most $β/δ$-type SySt.
description: 12 pages, 7 figures, 5 tables; To appear in MNRAS
title: ÐÐ²ÑÐ¾Ð¼Ð¾Ð±Ð¸Ð»ÑÐ½ÑÐ¹ Ð±ÐµÐ½Ð·Ð¸Ð½Ð¾Ð²ÑÐ¹ Ð´Ð²Ð¸Ð³Ð°ÑÐµÐ»Ñ Ð¼Ð¾ÑÐ½Ð¾ÑÑÑÑ 40 ÐºÐÑ
title: Ð±Ð°ÐºÐ°Ð»Ð°Ð²ÑÑÐºÐ°Ñ ÑÐ°Ð±Ð¾ÑÐ°
titleType: Subtitle
Creators: name: ÐÐ°ÑÐºÐ¸Ð½, ÐÑÑÐµÐ¼Ð¸Ð¹
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: Ð°Ð²ÑÐ¾Ð¼Ð¾Ð±Ð¸Ð»ÑÐ½ÑÐ¹ Ð±ÐµÐ½Ð·Ð¸Ð½Ð¾Ð²ÑÐ¹ Ð´Ð²Ð¸Ð³Ð°ÑÐµÐ»Ñ
ÑÐ°Ð±Ð¾ÑÐ¸Ð¹ Ð¿ÑÐ¾ÑÐµÑÑ
Ð¿ÑÐ¾ÑÐ½Ð¾ÑÑÐ½Ð¾Ð¹ ÑÐ°ÑÑÐµÑ

description: ÐÐ°Ð½Ð½Ð°Ñ ÑÐ°Ð±Ð¾ÑÐ° Ð¿Ð¾ÑÐ²ÑÑÐµÐ½Ð° ÑÐ°Ð·ÑÐ°Ð±Ð¾ÑÐºÐµ Ð°Ð²ÑÐ¾Ð¼Ð¾Ð±Ð¸Ð»ÑÐ½Ð¾Ð³Ð¾ Ð±ÐµÐ½Ð·Ð¸Ð½Ð¾Ð²Ð¾Ð³Ð¾ Ð´Ð²Ð¸Ð³Ð°ÑÐµÐ»Ñ Ð²Ð½ÑÑÑÐµÐ½Ð½ÐµÐ³Ð¾ ÑÐ³Ð¾ÑÐ°Ð½Ð¸Ñ Ð¼Ð¾ÑÐ½Ð¾ÑÑÑÑ 40 ÐºÐÑ. Ð ÑÐ¾Ð´Ðµ Ð²ÑÐ¿Ð¾Ð»Ð½ÐµÐ½Ð¸Ñ ÑÐ°Ð±Ð¾ÑÑ ÑÐ°ÑÑÑÐ¸ÑÐ°Ð½Ñ: ÑÐ°Ð±Ð¾ÑÐ¸Ð¹ Ð¿ÑÐ¾ÑÐµÑÑ Ð´Ð²Ð¸Ð³Ð°ÑÐµÐ»Ñ Ð¿Ð¾ Ð¼ÐµÑÐ¾Ð´Ñ ÐÑÐ¸Ð½ÐµÐ²ÐµÑÐºÐ¾Ð³Ð¾-ÐÐ°Ð·Ð¸Ð½Ð³Ð°, ÑÐ¸Ð»Ñ Ð¸ Ð¼Ð¾Ð¼ÐµÐ½ÑÑ, Ð²Ð¾Ð·Ð½Ð¸ÐºÐ°ÑÑÐ¸Ðµ Ð² ÑÐ»ÐµÐ¼ÐµÐ½ÑÐ°Ñ Ð´Ð²Ð¸Ð³Ð°ÑÐµÐ»Ñ, Ð° ÑÐ°ÐºÐ¶Ðµ Ð¿ÑÐ¾Ð¸Ð·Ð²ÐµÐ´ÐµÐ½ Ð°Ð½Ð°Ð»Ð¸Ð· ÑÑÐ°Ð²Ð½Ð¾Ð²ÐµÑÐµÐ½Ð½Ð¾ÑÑÐ¸ Ð¸ Ð²ÑÐ¿Ð¾Ð»Ð½ÐµÐ½Ñ ÑÐ°ÑÑÐµÑÑ Ð¿ÑÐ¾ÑÐ½Ð¾ÑÑÐ¸ ÐºÐ¾Ð»ÐµÐ½ÑÐ°ÑÐ¾Ð³Ð¾ Ð²Ð°Ð»Ð°, ÑÐ°ÑÑÐ½Ð° Ð¸ Ð¿Ð¾ÑÑÐ½ÐµÐ²Ð¾Ð³Ð¾ Ð¿Ð°Ð»ÑÑÐ° Ð´Ð²Ð¸Ð³Ð°ÑÐµÐ»Ñ. ÐÐ° Ð¾ÑÐ½Ð¾Ð²Ð°Ð½Ð¸Ð¸ ÑÐ°ÑÑÐµÑÐ¾Ð² ÑÐ°Ð·ÑÐ°Ð±Ð¾ÑÐ°Ð½Ñ Ð¿ÑÐ¾Ð´Ð¾Ð»ÑÐ½ÑÐ¹ Ð¸ Ð¿Ð¾Ð¿ÐµÑÐµÑÐ½ÑÐ¹ ÑÐ°Ð·ÑÐµÐ·Ñ Ð´Ð²Ð¸Ð³Ð°ÑÐµÐ»Ñ.
SDSS-IV MaNGA: The Incidence of Major Mergers in type I and II AGN Host Galaxies in the DR15 sample
Creators: name: Hernández-Toledo, Héctor
name: Cortes-Suárez, Edgar
name: Vázquez-Mata, Jose Antonio
name: Nevin, Rebecca
name: Ávila-Reese, Vladimir
name: Ibarra-Medel, Héctor
name: Negrete, Alenka
Publisher: name: arXiv
Year: 2023
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: We present a study on the incidence of major mergers and their impact on the triggering of nuclear activity in 47 type I and 236 type II optically-selected AGN from the MaNGA DR15 sample. From an estimate of non-parametric image predictors ($Gini$, M$_{20}$, concentration (C), asymmetry (A), clumpiness (S), Sérsic index (n), and shape asymmetry($A_S$)) using the SDSS images, in combination with a Linear Discriminant Analysis Method, we identified major mergers and merger stages. We reinforced our results by looking for bright tidal features in our post-processed SDSS and DESI legacy images. We find a statistically significant higher incidence of major mergers of 29\% $\pm$ 3\% in our type I+II AGN sample compared to 22\% $\pm$ 0.8\% for a non-AGN sample matched in redshift, stellar mass, color and morphological type, finding also a prevalence of post-coalescence (51\% $\pm$ 5\%) over pre-coalescence (23\% $\pm$ 6\%) merger stages. The levels of AGN activity among our massive major mergers are similar to those reported in other works using \oiii\ tracers. However, similar levels are produced by our AGN-galaxies hosting stellar bars, suggesting that major mergers are important promoters of nuclear activity but are not the main nor the only mechanism behind the AGN triggering. The tidal strength parameter $Q$ was considered at various scales looking for environmental differences that could affect our results on the merger incidence, finding non-significant differences. Finally, the H-H$β$ diagram could be used as an empirical predictor for the flux coming from an AGN source, useful to correct photometric quantities in large AGN samples emerging from surveys.
description: 23 pages, 13 figures, 10 tables
Onthophagus velutinus Horn 1875
Creators: name: Kohlmann, Bert
name: Solís, Ángel
Publisher: name: Zenodo
Year: 2025
Subjects: Biodiversity
Taxonomy
Animalia
Arthropoda
Insecta
Coleoptera
Scarabaeidae
Onthophagus
Onthophagus velutinus

description: Onthophagus velutinus species group*.
This group is diagnosed by a pronotal disc distinctly tuberculate; clypeus slightly emarginate; surface of pronotum and (or) elytra finely alutaceous. Male with two straight and erect horns at vertex (Figs. 5.19 –20); male protibia short and stout (Figs. 1.29 –30); male protibial spur inwardly bent at apex (Figs. 1.29 –30); male protibial apex with some short setae (Figs. 1.29 –30); metafemur long and slender (Figs. 2.29 –30); male pronotum with a well-developed central gibbosity (Figs. 5.19 –20); apex of parameres well developed and defined. Females with carina of vertex nearly straight.
Zunino & Halffter (1997: 159) included O. velutinus Horn as part of the O. mexicanus species group without giving any justification for this decision. Later, Zunino (2003) considered O. cartwrighti Howden to be in an incertae sedis species group. Subsequently, Moctezuma & Halffter (2019) suggested that O. cartwrighti should be included within the O. mexicanus species group due to its close relationship to O. velutinus. We disagree with these opinions because these species have a different Bauplan (from the German, Bauplan (s.) [Baupläne, pl.], body plan, a suite of characters shared by a group of phylogenetically related animals at some point during their development; Willmore 2012) from the O. mexicanus species group.
While the mtDNA analyses suggested a relationship between the O. velutinus and O. mexicanus species groups (Figs. 1–2, 8–9), the external morphological Bauplan between these two groups is entirely different. The O. velutinus species group, contrary to the O. mexicanus species group, does not have pronotal horns and no short and thick metafemora (Figs. 2.29 –30) and presents very characteristic and almost parallel long vertex horns (Figs. 5.19 –20). Howden & Cartwright (1963: 107) indicated that O. velutinus is quite distinct from other Western Hemispheric Onthophagus species and seemed restricted to Neotoma Say & Ord (Rodentia: Cricetidae) nests. We suggest that O. cartwrighti and O. velutinus form a new species group, the O. velutinus species group, distributed in the Southwestern United States of America and the Baja California Peninsula.
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 pages 429-430, DOI: 10.11646/zootaxa.5604.4.1, http://zenodo.org/record/15213967
Review of Observational Evidence for Dark Matter in the Universe and in upcoming searches for Dark Stars
Creators: name: Freese, Katherine
Publisher: name: arXiv
Year: 2008
Subjects: subject: Astrophysics (astro-ph)
subject: High Energy Physics - Phenomenology (hep-ph)
subject: FOS: Physical sciences

description: Over the past decade, a consensus picture has emerged in which roughly a quarter of the universe consists of dark matter. The observational evidence for the existence of dark matter is reviewed: rotation curves of galaxies, weak lensing measurements, hot gas in clusters, primordial nucleosynthesis and microwave background experiments. In addition, a new line of research on Dark Stars is presented, which suggests that the first stars to exist in the universe were powered by dark matter heating rather than by fusion: the observational possibilities of discovering dark matter in this way are discussed.
description: 14 pages, 7 figures, Conference Proceeding for "Dark Matter and Dark Energy" in Lyon, France, July 2008
Generalized Toffoli gates using qudit catalysis
Creators: name: Ionicioiu, Radu
name: Spiller, Timothy P.
name: Munro, William J.
Publisher: name: arXiv
Year: 2009
Subjects: subject: Quantum Physics (quant-ph)
subject: FOS: Physical sciences

description: We present quantum networks for a n-qubit controlled gate C^{n-1}(U) which use a higher dimensional (qudit) ancilla as a catalyser. In its simplest form the network has only n two-particle gates (qubit-qudit) -- this is the minimum number of two-body interactions needed to couple all n+1 subsystems (n qubits plus one ancilla). This class of controlled gates includes the generalised Toffoli gate C^{n-1}(X) on n qubits, which plays an important role in several quantum algorithms and error correction. A particular example implementing this model is given by the dispersive limit of a generalised Jaynes-Cummings Hamiltonian of an effective spin-s interacting with a cavity mode.
description: 5 pages, 3 figs