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47
Jul 20, 2013
07/13
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Y. Xin; L. Deng; Z. Han
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eye 47
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Blue straggler stars present as secure members in the Galactic open clusters form a major challenge to the conventional picture of evolutionary population synthesis based on the stellar evolution theory of single stars, as illustrated in our previous work. Expansion of our sample in the current work to include younger age clusters provides a larger data base to expose the question raised for the simple stellar population model. The working sample now includes 97 Galactic open clusters of ages...
Source: http://arxiv.org/abs/astro-ph/0609745v1
2
2.0
Jun 28, 2018
06/18
by
Z. Han; M. Lu
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eye 2
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Let $\chi'_d(n,q)$ (resp. $\chi_d(n,q)$) denote the minimum number of colors necessary to color a $q$-ary $n$-cube so that no two vertices that are at a distance at most $d$ (resp. exactly $d$) get the same color. These two problems were proposed in the study of scalability of optical networks. In this paper, we provide upper and lower bounds on $\chi'_d(n,q)$ and $\chi_d(n,q)$ when $q$ is a prime power.
Topics: Combinatorics, Mathematics
Source: http://arxiv.org/abs/1510.08168
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2.0
Jun 30, 2018
06/18
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F. Zhang; L. Li; L. Cheng; L. Wang; X. Kang; Y. Zhuang; Z. Han
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eye 2
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Radiation fields emitted by O, B-type stars or young stellar populations (SPs) are generally considered as significant central ionizing sources (CISs) of classic H II regions. In our previous studies, we show that the inclusion of binary interactions in stellar population synthesis models can significantly increase the ultraviolet spectrum hardness and the number of ionizing photons of intermediate-age (IA, 7
Topics: Astrophysics, Solar and Stellar Astrophysics
Source: http://arxiv.org/abs/1410.6544
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8.0
Jun 27, 2018
06/18
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S. Geier; F. Fürst; E. Ziegerer; T. Kupfer; U. Heber; A. Irrgang; B. Wang; Z. Liu; Z. Han; B. Sesar; D. Levitan; R. Kotak; E. Magnier; K. Smith; W. S. Burgett; K. Chambers; H. Flewelling; N. Kaiser; R. Wainscoat; C. Waters
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Hypervelocity stars (HVS) travel with velocities so high, that they exceed the escape velocity of the Galaxy. Several acceleration mechanisms have been discussed. Only one HVS (US 708, HVS 2) is a compact helium star. Here we present a spectroscopic and kinematic analysis of US\,708. Travelling with a velocity of $\sim1200\,{\rm km\,s^{-1}}$, it is the fastest unbound star in our Galaxy. In reconstructing its trajectory, the Galactic center becomes very unlikely as an origin, which is hardly...
Topics: Solar and Stellar Astrophysics, Astrophysics
Source: http://arxiv.org/abs/1503.01650
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6.0
Jun 28, 2018
06/18
by
D. Niyato; X. Lu; P. Wang; D. I. Kim; Z. Han
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eye 6
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Internet of things (IoT) has been proposed to be a new paradigm of connecting devices and providing services to various applications, e.g., transportation, energy, smart city, and healthcare. In this paper, we focus on an important issue, i.e., economics of IoT, that can have a great impact to the success of IoT applications. In particular, we adopt and present the information economics approach with its applications in IoT. We first review existing economic models developed for IoT services....
Topics: Networking and Internet Architecture, Computing Research Repository
Source: http://arxiv.org/abs/1510.06837
2
2.0
Jun 30, 2018
06/18
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S. Linas; Y. Magnin; B. Poinsot; O. Boisron; G. D. Forster; Z. Han; D. Kalita; V. Bouchiat; V. Martinez; R. Fulcrand; F. Tournus; V. Dupuis; F. Rabilloud; L. Bardotti; F. Calvo
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eye 2
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Measurements and calculations have shown significant disagreement regarding the sign and variations of the thermal expansion coefficient (TEC) of graphene $\alpha(T)$. Here we report dedicated Raman scattering experiments conducted for graphene monolayers deposited on silicon nitride substrates and over the broad temperature range 150--900~K. The relation between those measurements for the G band and the graphene TEC, which involves correcting the measured signal for the mismatch contribution...
Topics: Mesoscale and Nanoscale Physics, Materials Science, Condensed Matter
Source: http://arxiv.org/abs/1411.7840
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3.0
Jun 30, 2018
06/18
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F. Lafont; R. Ribeiro-Palau; Z. Han; A. Cresti; A. Delvallée; A. W. Cummings; S. Roche; V. Bouchiat; S. Ducourtieux; F. Schopfer; W. Poirier
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eye 3
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We report on the observation of strong backscattering of charge carriers in the quantum Hall regime of polycrystalline graphene grown by chemical vapor deposition, which alters the accuracy of the Hall resistance quantization. The temperature and magnetic field dependence of the longitudinal conductivity exhibits unexpectedly smooth power law behaviors, which are incompatible with a description in terms of variable range hopping or thermal activation, but rather suggest the existence of...
Topics: Mesoscale and Nanoscale Physics, Condensed Matter
Source: http://arxiv.org/abs/1404.2536
2
2.0
Jun 29, 2018
06/18
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H. Xiong; X. Chen; P. Podsiadlowski; Y. Li; Z. Han
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eye 2
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From the canonical binary scenario, the majority of sdBs are produced from low-mass stars with degenerate cores where helium is ignited in a way of flashes. Due to numerical difficulties, the models of produced sdBs are generally constructed from more massive stars with non-degenerate cores, leaving several uncertainties on the exact characteristics of sdB stars. Employing MESA, we systematically studied the characteristics of sdBs produced from the common envelope (CE) ejection channel, and...
Topics: Astrophysics, Solar and Stellar Astrophysics
Source: http://arxiv.org/abs/1608.08739
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68
Sep 22, 2013
09/13
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S. B. Pu; R. P. Saglia; M. H. Fabricius; J. Thomas; R. Bender; Z. Han
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eye 68
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We present high quality long slit spectra along the major and minor axes out to 1.5-2 Re (14-22 kpc) of three bright elliptical galaxies (NGC1600, NGC4125, NGC7619) obtained at the Hobby-Eberly Telescope (HET). We derive stellar kinematic profiles and Lick/IDS indices (Hbeta, Mgb, Fe5015, Fe5270, Fe5335, Fe5406). Moreover, for NGC4125 we derive gas kinematics and emission line strengths. We model the absorption line strengths using Simple Stellar Populations models that take into account the...
Source: http://arxiv.org/abs/1004.2776v1
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3.0
Jun 30, 2018
06/18
by
T. R. Zhan; D. Z. Han; X. H. Hu; X. H. Liu; S. T. Chui; J. Zi
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eye 3
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Based on a structure consisting of a single graphene layer situated on a periodic dielectric grating, we show theoretically that intense terahertz (THz) radiations can be generated by an electron bunch moving atop the graphene layer. The underlying physics lies in the fact that a moving electron bunch with rather low electron energy ($\sim$1 keV) can efficiently excite graphene plasmons (GPs) of THz frequencies with a strong confinement of near-fields. GPs can be further scattered into free...
Topics: Mesoscale and Nanoscale Physics, Condensed Matter
Source: http://arxiv.org/abs/1402.2829
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93
Sep 18, 2013
09/13
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N. Ivanova; S. Justham; X. Chen; O. De Marco; C. L. Fryer; E. Gaburov; H. Ge; E. Glebbeek; Z. Han; X. -D. Li; G. Lu; T. Marsh; Ph. Podsiadlowski; A. Potter; N. Soker; R. Taam; T. M. Tauris; E. P. J. van den Heuvel; R. F. Webbink
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eye 93
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This work aims to present our current best physical understanding of common-envelope evolution (CEE). We highlight areas of consensus and disagreement, and stress ideas which should point the way forward for progress in this important but long-standing and largely unconquered problem. Unusually for CEE-related work, we mostly try to avoid relying on results from population synthesis or observations, in order to avoid potentially being misled by previous misunderstandings. As far as possible we...
Source: http://arxiv.org/abs/1209.4302v2
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46
Sep 22, 2013
09/13
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L. G. Althaus; A. H. Corsico; A. Gautschy; Z. Han; A. M. Serenelli; J. A. Panei
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eye 46
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The present work is designed to explore the evolutionary and pulsational properties of low-mass white dwarfs with carbon/oxygen cores. In particular, we follow the evolution of a 0.33 Msun white dwarf remnant in a self-consistent way with the predictions of nuclear burning, element diffusion and the history of the white dwarf progenitor. Attention is focused on the occurrence of hydrogen shell flashes induced by diffusion processes during cooling phases. The evolutionary stages prior to the...
Source: http://arxiv.org/abs/astro-ph/0309276v1
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34
Sep 21, 2013
09/13
by
S. B. Pu; Z. Han
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eye 34
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We present high quality long slit spectra along the major and minor axes out to 1.5 effective radius ($R_e$) of the massive galaxy NGC4636 taken by Hobby-Eberly Telescope (HET). Using Fourier Correlation Quotient (FCQ) method, we measured the stellar line-of-sight velocity distribution along the axes. Furthermore, six Lick/IDS indices ($H\beta,Mgb,Fe_{5015},Fe_{5270},Fe_{5335},Fe_{5406}$) are derived from the clean spectrum. By comparing the measured absorption line strengths with the...
Source: http://arxiv.org/abs/1104.4845v1
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48
Sep 21, 2013
09/13
by
X. Meng; X. Chen; Z. Han
texts
eye 48
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Using a simple analytic method, we calculate the impact effect between the ejecta of a SN Ia and its companion to survey the influence of initial parameters of the progenitor's system, which is useful for searching the companion in a explosion remnant. The companion models are obtained from Eggleton's evolution code.The results are divided into two groups based on mass transfer stage. For a given condition, more hydrogen-rich material is stripped from the envelope of a Hertzsprung-gap companion...
Source: http://arxiv.org/abs/0706.3581v1
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101
Sep 18, 2013
09/13
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O. R. Pols; C. A. Tout; P. P. Eggleton; Z. Han
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eye 101
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We present a simple and efficient, yet reasonably accurate, equation of state, which at the moderately low temperatures and high densities found in the interiors of stars less massive than the Sun is substantially more accurate than its predecessor by Eggleton, Faulkner & Flannery. Along with the most recently available values in tabular form of opacities, neutrino loss rates, and nuclear reaction rates for a selection of the most important reactions, this provides a convenient package of...
Source: http://arxiv.org/abs/astro-ph/9504025v1
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66
Sep 22, 2013
09/13
by
F. Zhang; L. Li; Z. Han; Y. Zhuang; X. Kang
texts
eye 66
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We build the Yunnan-III evolutionary population synthesis (EPS) models by using the MESA stellar evolution code, BaSeL stellar spectra library and the initial mass functions (IMFs) of Kroupa and Salpeter, and present colours and integrated spectral energy distributions (ISEDs) of solar-metallicity stellar populations (SPs) in the range of 1Myr-15 Gyr. The main characteristic of the Yunnan-III EPS models is the usage of a set of self-consistent solar-metallicity stellar evolutionary tracks (the...
Source: http://arxiv.org/abs/1210.6452v1
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38
Sep 19, 2013
09/13
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Z. Han; X. Chen; F. Zhang; Ph. Podsiadlowski
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eye 38
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Most stars are members of binaries, and the evolution of a star in a close binary system differs from that of an ioslated star due to the proximity of its companion star. The components in a binary system interact in many ways and binary evolution leads to the formation of many peculiar stars, including blue stragglers and hot subdwarfs. We will discuss binary evolution and the formation of blue stragglers and hot subdwarfs, and show that those hot objects are important in the study of...
Source: http://arxiv.org/abs/0910.2546v1
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38
Sep 19, 2013
09/13
by
X. Chen; Z. Han
texts
eye 38
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Blue stragglers have been found in all populations. These objects are important in both stellar evolution and stellar population synthesis. Much evidence shows that blue stragglers are relevant to primordial binaries. Here, we summarize the links of binary evolution and blue stragglers, describe the characteristics of blue stragglers from different binary evolutionary channels, and show their consequences for binary population synthesis, such as for the integrated spectral energy distribution,...
Source: http://arxiv.org/abs/0910.2545v1
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39
Sep 22, 2013
09/13
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T. Lisker; U. Heber; R. Napiwotzki; N. Christlieb; Z. Han; D. Homeier; D. Reimers
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eye 39
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We present the analysis of a high-resolution, high-quality sample of optical spectra for 76 subdwarf B (sdB) stars from the ESO Supernova Ia Progenitor Survey (SPY). Effective temperature, surface gravity, and photospheric helium abundance are determined simultaneously by fitting the profiles of hydrogen and helium lines using synthetic spectra calculated from LTE and NLTE model atmospheres. We perform a detailed comparison of our measurements with theoretical calculations, both for single star...
Source: http://arxiv.org/abs/astro-ph/0409136v2
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50
Sep 22, 2013
09/13
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P. F. L. Maxted; T. R. Marsh; C. K. J. Moran; Z. Han
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eye 50
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WD1704+481 is a visual binary in which both components are white dwarfs. We present spectra of the H-alpha line of both stars which show that one component (WD1704+481.2 = Sanduleak B = GR 577) is a close binary with two white dwarf components. Thus, WD1704+481 is the first known triple degenerate star. From radial velocity measurements of the close binary we find an orbital period of 0.1448d, a mass ratio, q=Mbright/Mfaint of q=0.70+-0.03 and a difference in the gravitational redshifts of...
Source: http://arxiv.org/abs/astro-ph/0001212v2
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51
Sep 22, 2013
09/13
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Z. H. Zhang; D. J. Pinfield; A. C. Day-Jones; B. Burningham; H. R. A. Jones; S. Yu; J. S. Jenkins; Z. Han; M. C. Galvez-Ortiz; J. Gallardo; A. E. Garcia Perez; D. Weights; C. G. Tinney; R. S. Pokorny
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eye 51
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We identify 806 ultra-cool dwarfs from their SDSS riz photometry (of which 34 are newly discovered L dwarfs) and obtain proper motions through cross matching with UKIDSS and 2MASS. Proper motion and distance constraints show that nine of our ultra-cool dwarfs are members of widely separated binary systems; SDSS 0101 (K5V+M9.5V), SDSS 0207 (M1.5V+L3V), SDSS 0832 (K3III+L3.5V), SDSS 0858 (M4V+L0V), SDSS 0953 (M4V+M9.5V), SDSS 0956 (M2V+M9V), SDSS 1304 (M4.5V+L0V), SDSS 1631 (M5.5V+M8V), SDSS 1638...
Source: http://arxiv.org/abs/1001.3609v1
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60
Sep 21, 2013
09/13
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Z. H. Zhang; R. S. Pokorny; H. R. A. Jones; D. J. Pinfield; P. S. Chen; Z. Han; D. Chen; M. C. Gálvez-Ortiz; B. Burningham
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eye 60
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Aims. We try to identify ultra-cool dwarfs from the seventh Data Release of the Sloan Digital Sky Survey (SDSS DR7) with SDSS i-z and r-z colors. We also obtain proper motion data from SDSS, 2MASS, and UKIDSS and improve spectral typing from SDSS and 2MASS photometric colors. Methods. We selected ultra-cool dwarf candidates from the SDSS DR7 with new photometric selection criteria, which are based on a parameterization study of known L and T dwarfs. The objects are then cross-identified with...
Source: http://arxiv.org/abs/0902.2798v1
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32
Sep 23, 2013
09/13
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Ph. Podsiadlowski; Z. Han; S. Rappaport
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eye 32
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We present the results of a systematic study of cataclysmic variables (CVs) and related systems, combining detailed binary-population synthesis (BPS) models with a grid of 120 binary evolution sequences calculated with a Henyey-type stellar evolution code. In these sequences, we used 3 masses for the white dwarf (0.6, 0.8, 1.0 Msun) and seven masses for the donor star in the range of 0.6-1.4 Msun. The shortest orbital periods were chosen to have initially unevolved secondaries, and the longest...
Source: http://arxiv.org/abs/astro-ph/0109171v1
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43
Sep 23, 2013
09/13
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F. Zhang; Z. Han; L. Li; Y. Zhang; J. Guo
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eye 43
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Subdwarf B stars (sdBs) can significantly change the ultraviolet spectra of populations at age t~1Gyr, and have been even included in the volutionary population synthesis (EPS) models by Han et al. (2007). In this study we present the spectral energy distributions (SEDs) of binary stellar populations (BSPs) by combining the EPS models of Han et al. (2007) and those of the Yunnan group (Zhang et al. 2004, 005), which have included various binary interactions (except sdBs) in EPS models. This set...
Source: http://arxiv.org/abs/1006.3975v2
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84
Jul 20, 2013
07/13
by
Z. Han
texts
eye 84
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The binary fraction among extreme horizontal branch (EHB) stars in Galactic globular clusters (GCs) is an order of magnitude lower than the binary fraction among their counterparts, field hot subdwarfs. This casts serious doubt on their formation channels. In this {\em Letter}, I explain the difference between the field and the cluster EHB stars with the binary model of Han et al. (2002, 2003) for the formation of EHB stars. With the binary population synthesis code of Han et al. (2002, 2003),...
Source: http://arxiv.org/abs/0804.4535v2
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114
Sep 23, 2013
09/13
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F. Zhang; L. Li; Z. Han
texts
eye 114
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In our evolutionary population synthesis models, the samples of binaries are reproduced by the 'patched' Monte Carlo simulation and the stellar masses, integrated J, H, K, L, L2 and M magnitudes, mass-to-light ratios and broad colours involving infrared bands are presented, for an extensive set of instantaneous-burst binary stellar populations. In addition, the fluctuations in the integrated colours, which have been given by Zhang et al. (2005), are reduced. By comparing the results for binary...
Source: http://arxiv.org/abs/1006.3983v2
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78
Sep 23, 2013
09/13
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F. Zhang; Z. Han; L. Li; H. Shan; Y. Zhang
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eye 78
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Using the Hyperz code and a template spectral library which consists of 4 observed galaxy spectra from Coleman, Wu & Weedman (CWW, 1980) and 8 spectral families built with evolutionary population synthesis models, we present photometric redshift estimates (photo-z) for a spectroscopic sample of 6,531 galaxies, and morphologies for a morphological sample of 1,502 bright galaxies. All galaxies are matched with the SDSS DR7 and GALEX DR4. The inclusion of Fuv or Nuv or both photometry...
Source: http://arxiv.org/abs/1006.4416v1
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95
Jul 20, 2013
07/13
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B. Tian; L. Deng; Z. Han; X. B. Zhang
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eye 95
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In this paper, we present the simulations for the primordial blue stragglers in the old open cluster M67 based on detailed modelling of the evolutionary processes. The principal aim is to discuss the contribution of mass transfer between the components of close binaries to the blue straggler population in M67. First, we followed the evolution of a binary of 1.4M$_\odot$+0.9M$_\odot$. The synthetic evolutionary track of the binary system revealed that a primordial blue straggler had a long...
Source: http://arxiv.org/abs/astro-ph/0604290v2
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39
Sep 23, 2013
09/13
by
F. Zhang; L. Li; Z. Han
texts
eye 39
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We present the integrated J, H, K, L, M and N magnitudes and the colours involving infrared bands, for an extensive set of instantaneous-burst binary stellar populations (BSPs) by using evolutionary population synthesis (EPS). By comparing the results for BSPs WITH and WITHOUT binary interactions we show that the inclusion of binary interactions makes the magnitudes of populations larger (fainter) and the integrated colours smaller (bluer) for t > 1Gyr. Also, we compare our model magnitudes...
Source: http://arxiv.org/abs/1006.3590v2
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33
Sep 21, 2013
09/13
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B. Wang; X. Meng; X. Chen; Z. Han
texts
eye 33
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Type Ia supernovae (SNe Ia) play an important role in astrophysics, especially in the study of cosmic evolution. There are several progenitor models for SNe Ia proposed in the past years. In this paper, we have carried out a detailed study of the He star donor channel, in which a carbon-oxygen white dwarf (CO WD) accretes material from a He main sequence star or a He subgiant to increase its mass to the Chandrasekhar mass. Employing Eggleton's stellar evolution code with an optically thick wind...
Source: http://arxiv.org/abs/0901.3496v1
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38
Sep 22, 2013
09/13
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X. Chen; Z. Han
texts
eye 38
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We studied the effects of surface composition and thermohaline mixing caused by secular instability on the accreting components for low--mass binaries and applied the results on a short-orbital-period BS F190 in the old cluster M67. The results indicate no distinction in surface composition between the models with and without thermohaline mixing during Roche lobe overflow, but we still see the divergences of evolutionary tracks on HRD and CMD. The change of surface composition makes the gainer...
Source: http://arxiv.org/abs/astro-ph/0409607v1
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42
Sep 24, 2013
09/13
by
L. Li; Z. Han; F. Zhang
texts
eye 42
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In a preceding paper, using Eggleton's evolution code we have discussed the structure and evolution of low-mass W UMa type contact binaries without angular momentum loss (AML). The models exhibit cyclic behavior about a state of marginal contact on a thermal time-scale. Part of the time of each cycle is spent in contact and part in a semi-detached state. According to observations, W UMa systems suffer AML. We present the models of low-mass contact binaries with AML due to gravitational wave...
Source: http://arxiv.org/abs/astro-ph/0412072v1
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Jul 20, 2013
07/13
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S. Geier; T. R. Marsh; B. Wang; B. Dunlap; B. N. Barlow; V. Schaffenroth; X. Chen; A. Irrgang; P. F. L. Maxted; E. Ziegerer; T. Kupfer; B. Miszalski; U. Heber; Z. Han; A. Shporer; J. H. Telting; B. T. Gaensicke; R. H. Oestensen; S. J. O'Toole; R. Napiwotzki
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Type Ia supernovae (SN Ia) are the most important standard candles for measuring the expansion history of the universe. The thermonuclear explosion of a white dwarf can explain their observed properties, but neither the progenitor systems nor any stellar remnants have been conclusively identified. Underluminous SN Ia have been proposed to originate from a so-called double-detonation of a white dwarf. After a critical amount of helium is deposited on the surface through accretion from a close...
Source: http://arxiv.org/abs/1304.4452v1
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Sep 23, 2013
09/13
by
Zhen-Xin Lei; Xue-Fei Chen; Feng-Hui Zhang; Z. Han
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eye 42
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Metallicity is the first parameter to influence the horizontal branch (HB) morphology of globular clusters (GCs). It has been found, however, that some other parameters may also play an important role in affecting the morphology. While the nature of these important parameters remains unclear, they are believed to be likely correlated with wind mass-loss of red giants, since this mass loss determines their subsequent locations on the HB. Unfortunately, the mass loss during the red giant stages...
Source: http://arxiv.org/abs/1212.3063v1
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Sep 20, 2013
09/13
by
X. Meng; X. Chen; Z. Han
texts
eye 32
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The single-degenerate channel for the progenitors of type Ia supernovae (SNe Ia) are currently accepted, in which a carbon-oxygen white dwarf (CO WD) accretes hydrogen-rich material from its companion, increases its mass to the Chandrasekhar mass limit, and then explodes as a SN Ia. Incorporating the prescription of \citet{HAC99a} for the accretion efficiency into Eggleton's stellar evolution code and assuming that the prescription is valid for \emph{all} metallicities, we performed binary...
Source: http://arxiv.org/abs/0802.2471v2
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Sep 20, 2013
09/13
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P. Lesaffre; Z. Han; C. A. Tout; Ph. Podsiadlowski; R. G. Martin
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Thanks to a stellar evolution code able to compute through the C-flash we link the binary population synthesis of single degenerate progenitors of type Ia supernovae (SNe Ia) to their physical condition at the time of ignition. We show that there is a large range of possible ignition densities and we detail how their probability distribution depends on the accretion properties. The low density peak of this distribution qualitatively reminds of the clustering of the luminosities of Branch-normal...
Source: http://arxiv.org/abs/astro-ph/0601443v1
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7.0
Jun 28, 2018
06/18
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T. Adam; F. An; G. An; Q. An; N. Anfimov; V. Antonelli; G. Baccolo; M. Baldoncini; E. Baussan; M. Bellato; L. Bezrukov; J. Hu; S. Hu; T. Hu; W. Hu; H. Huang; X. Huang; X. Huang; L. Huo; W. Huo; A. Ioannisian; D. Bick; D. Ioannisyan; M. Jeitler; K. Jen; S. Jetter; X. Ji; X. Ji; S. Jian; D. Jiang; X. Jiang; C. Jollet; S. Blyth; M. Kaiser; B. Kan; L. Kang; M. Karagounis; N. Kazarian; S. Kettell; D. Korablev; A. Krasnoperov; S. Krokhaleva; Z. Krumshteyn; S. Boarin; A. Kruth; P. Kuusiniemi; T. Lachenmaier; L. Lei; R. Lei; X. Lei; R. Leitner; F. Lenz; C. Li; F. Li; A. Brigatti; F. Li; J. Li; N. Li; S. Li; T. Li; W. Li; W. Li; X. Li; X. Li; X. Li; T. Brugière; X. Li; Y. Li; Y. Li; Z. Li; H. Liang; H. Liang; J. Liang; M. Licciardi; G. Lin; S. Lin; R. Brugnera; T. Lin; Y. Lin; I. Lippi; G. Liu; H. Liu; H. Liu; J. Liu; J. Liu; J. Liu; J. Liu; M. Buizza Avanzini; Q. Liu; Q. Liu; S. Liu; S. Liu; Y. Liu; P. Lombardi; Y. Long; S. Lorenz; C. Lu; F. Lu; J. Busto; H. Lu; J. Lu; J. Lu; J. Lu; B. Lubsandorzhiev; S. Lubsandorzhiev; L. Ludhova; F. Luo; S. Luo; Z. Lv; A. Cabrera; V. Lyashuk; Q. Ma; S. Ma; X. Ma; X. Ma; Y. Malyshkin; F. Mantovani; Y. Mao; S. Mari; D. Mayilyan; H. Cai; W. McDonough; G. Meng; A. Meregaglia; E. Meroni; M. Mezzetto; J. Min; L. Miramonti; M. Montuschi; N. Morozov; T. Mueller; X. Cai; P. Muralidharan; M. Nastasi; D. Naumov; E. Naumova; I. Nemchenok; Z. Ning; H. Nunokawa; L. Oberauer; J. P. Ochoa-Ricoux; A. Olshevskiy; A. Cammi; F. Ortica; H. Pan; A. Paoloni; N. Parkalian; S. Parmeggiano; V. Pec; N. Pelliccia; H. Peng; P. Poussot; S. Pozzi; D. Cao; E. Previtali; S. Prummer; F. Qi; M. Qi; S. Qian; X. Qian; H. Qiao; Z. Qin; G. Ranucci; A. Re; G. Cao; B. Ren; J. Ren; T. Rezinko; B. Ricci; M. Robens; A. Romani; B. Roskovec; X. Ruan; X. Ruan; A. Rybnikov; J. Cao; A. Sadovsky; P. Saggese; G. Salamanna; J. Sawatzki; J. Schuler; A. Selyunin; G. Shi; J. Shi; Y. Shi; V. Sinev; J. Chang; C. Sirignano; M. Sisti; O. Smirnov; M. Soiron; A. Stahl; L. Stanco; J. Steinmann; V. Strati; G. Sun; X. Sun; Y. Chang; Y. Sun; Y. Sun; D. Taichenachev; J. Tang; A. Tietzsch; I. Tkachev; W. H. Trzaska; Y. Tung; S. van Waasen; C. Volpe; M. Chen; V. Vorobel; L. Votano; C. Wang; C. Wang; C. Wang; G. Wang; H. Wang; M. Wang; R. Wang; S. Wang; P. Chen; W. Wang; W. Wang; Y. Wang; Y. Wang; Y. Wang; Y. Wang; Z. Wang; Z. Wang; Z. Wang; Z. Wang; Q. Chen; Z. Wang; W. Wei; Y. Wei; M. Weifels; L. Wen; Y. Wen; C. Wiebusch; S. Wipperfurth; S. C. Wong; B. Wonsak; S. Chen; C. Wu; Q. Wu; Z. Wu; M. Wurm; J. Wurtz; Y. Xi; D. Xia; J. Xia; M. Xiao; Y. Xie; S. Chen; J. Xu; J. Xu; L. Xu; Y. Xu; B. Yan; X. Yan; C. Yang; C. Yang; H. Yang; L. Yang; S. Chen; M. Yang; Y. Yang; Y. Yang; Y. Yang; E. Yanovich; Y. Yao; M. Ye; X. Ye; U. Yegin; F. Yermia; X. Chen; Z. You; B. Yu; C. Yu; C. Yu; G. Yu; Z. Yu; Y. Yuan; Z. Yuan; M. Zanetti; P. Zeng; Y. Chen; S. Zeng; T. Zeng; L. Zhan; C. Zhang; F. Zhang; G. Zhang; H. Zhang; J. Zhang; J. Zhang; J. Zhang; Y. Cheng; K. Zhang; P. Zhang; Q. Zhang; T. Zhang; X. Zhang; X. Zhang; Y. Zhang; Y. Zhang; Y. Zhang; Y. Zhang; D. Chiesa; Y. Zhang; Y. Zhang; Z. Zhang; Z. Zhang; J. Zhao; M. Zhao; T. Zhao; Y. Zhao; H. Zheng; M. Zheng; A. Chukanov; X. Zheng; Y. Zheng; W. Zhong; G. Zhou; J. Zhou; L. Zhou; N. Zhou; R. Zhou; S. Zhou; W. Zhou; M. Clemenza; X. Zhou; Y. Zhou; H. Zhu; K. Zhu; H. Zhuang; L. Zong; J. Zou; B. Clerbaux; D. D'Angelo; H. de Kerret; Z. Deng; Z. Deng; X. Ding; Y. Ding; Z. Djurcic; S. Dmitrievsky; M. Dolgareva; D. Dornic; E. Doroshkevich; M. Dracos; O. Drapier; S. Dusini; M. A. Díaz; T. Enqvist; D. Fan; C. Fang; J. Fang; X. Fang; L. Favart; D. Fedoseev; G. Fiorentini; R. Ford; A. Formozov; R. Gaigher; H. Gan; A. Garfagnini; G. Gaudiot; C. Genster; M. Giammarchi; F. Giuliani; M. Gonchar; G. Gong; H. Gong; M. Gonin; Y. Gornushkin; M. Grassi; C. Grewing; V. Gromov; M. Gu; M. Guan; V. Guarino; W. Guo; X. Guo; Y. Guo; M. Göger-Neff; P. Hackspacher; C. Hagner; R. Han; Z. Han; J. Hao; M. He; D. Hellgartner; Y. Heng; D. Hong; S. Hou; Y. Hsiung; B. Hu
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The Jiangmen Underground Neutrino Observatory (JUNO) is proposed to determine the neutrino mass hierarchy using an underground liquid scintillator detector. It is located 53 km away from both Yangjiang and Taishan Nuclear Power Plants in Guangdong, China. The experimental hall, spanning more than 50 meters, is under a granite mountain of over 700 m overburden. Within six years of running, the detection of reactor antineutrinos can resolve the neutrino mass hierarchy at a confidence level of...
Topics: Instrumentation and Detectors, Physics, High Energy Physics - Experiment
Source: http://arxiv.org/abs/1508.07166
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Jun 28, 2018
06/18
by
A. Rebassa-Mansergas; M. Rybicka; X. -W. Liu; Z. Han; E. Garcia-Berro
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The mass function of hydrogen-rich atmosphere white dwarfs has been frequently found to reveal a distinctive high-mass excess near 1Msun. However, a significant excess of massive white dwarfs has not been detected in the mass function of the largest white dwarf catalogue to date from the Sloan Digital Sky Survey. Hence, whether a high-mass excess exists or not has remained an open question. In this work we build the mass function of the latest catalogue of data release 10 SDSS hydrogen-rich...
Topics: Solar and Stellar Astrophysics, Astrophysics
Source: http://arxiv.org/abs/1506.06802
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77
Sep 23, 2013
09/13
by
F. Zhang; L. Li; Z. Han
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Using the Hyperz code (Bolzonella et al. 2000) we present photometric redshift estimates for a random sample of galaxies selected from the SDSS/DR7 and GALEX/DR4, for which spectroscopic redshifts are also available. We confirm that the inclusion of ultraviolet photometry improves the accuracy of photo-zs for those galaxies with g*-r* < 0.7 and z_spec < 0.2. We also address the problem of how binary interactions can affect photo-z estimates, and find that their effect is negligible.
Source: http://arxiv.org/abs/1006.3588v2
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44
Sep 23, 2013
09/13
by
F. Zhang; Z. Han; L. Li
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eye 44
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Using Yunnan evolutionary population synthesis (EPS) models, we present integrated colours, integrated spectral energy distributions (ISEDs) and absorption-line indices defined by the Lick Observatory image dissector scanner (Lick/IDS) system, for an extensive set of instantaneous-burst binary stellar populations (BSPs) with interactions. By comparing the results for populations with and without interactions we show that the inclusion of binary interactions makes the appearance of the...
Source: http://arxiv.org/abs/1006.3593v2
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33
Sep 19, 2013
09/13
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Z. Han; Ph. Podsiadlowski; A. E. Lynas-Gray; K. Schawinski
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The discovery of an excess of light in the far-ultraviolet (UV) in 1969 in elliptical galaxies was a major surprise. While it is now clear that this UV excess (UV-upturn) is probably caused by an old population of helium-burning stars. Han et al (2002, 2003) proposed a binary model for the formation of hot subdwarfs (helium burning stars) and the model can reproduce the observations in our Galaxy. By applying the binary model to the study of evolutionary population synthesis, we have obtained...
Source: http://arxiv.org/abs/astro-ph/0703389v1
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40
Sep 19, 2013
09/13
by
X. Zhang; X. Chen; Z. Han
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eye 40
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Masses are a fundamental parameter, but they are not well known for most hot subdwarfs. In general, the mass of a hot subdwarf is derived with asteroseismology or dynamical methods, for which it is often difficult to obtain the necessary data from observations. We intend to find an approach to deriving the masses of hot subdwarfs from observational data in the literature. We presented full evolutionary calculations for hot subdwarfs in a wide mass range (0.33 $M_\odot$ to 1.4 $M_\odot$) for a...
Source: http://arxiv.org/abs/0909.2560v1
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18
Jun 27, 2018
06/18
by
D. Adams; A. Arce; L. Asquith; M. Backovic; T. Barillari; P. Berta; D. Bertolini; A. Buckley; J. Butterworth; R. C. Camacho Toro; J. Caudron; Y. -T. Chien; J. Cogan; B. Cooper; D. Curtin; C. Debenedetti; J. Dolen; M. Eklund; S. El Hedri; S. D. Ellis; T. Embry; D. Ferencek; J. Ferrando; S. Fleischmann; M. Freytsis; M. Giulini; Z. Han; D. Hare; P. Harris; A. Hinzmann; R. Hoing; A. Hornig; M. Jankowiak; K. Johns; G. Kasieczka; R. Kogler; W. Lampl; A. J. Larkoski; C. Lee; R. Leone; P. Loch; D. Lopez Mateos; H. K. Lou; M. Low; P. Maksimovic; I. Marchesini; S. Marzani; L. Masetti; R. McCarthy; S. Menke; D. W. Miller; K. Mishra; B. Nachman; P. Nef; F. T. O'Grady; A. Ovcharova; A. Picazio; C. Pollard; B. Potter-Landua; C. Potter; S. Rappoccio; J. Rojo; J. Rutherfoord; G. P. Salam; R. M. Schabinger; A. Schwartzman; M. D. Schwartz; B. Shuve; P. Sinervo; D. Soper; D. E. Sosa Corral; M. Spannowsky; E. Strauss; M. Swiatlowski; J. Thaler; C. Thomas; E. Thompson; N. V. Tran; J. Tseng; E. Usai; L. Valery; J. Veatch; M. Vos; W. Waalewijn; J. Wacker; C. Young
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Over the past decade, a large number of jet substructure observables have been proposed in the literature, and explored at the LHC experiments. Such observables attempt to utilize the internal structure of jets in order to distinguish those initiated by quarks, gluons, or by boosted heavy objects, such as top quarks and W bosons. This report, originating from and motivated by the BOOST2013 workshop, presents original particle-level studies that aim to improve our understanding of the...
Topics: High Energy Physics - Experiment, High Energy Physics - Phenomenology
Source: http://arxiv.org/abs/1504.00679
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39
Sep 20, 2013
09/13
by
F. Förster; C. Wolf; Ph. Podsiadlowski; Z. Han
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eye 39
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We re-assess the question of a systematic time delay between the formation of the progenitor and its explosion in a type Ia supernova (SN Ia) using the Hubble Higher-z Supernova Search sample (Strolger et al. 2004). While the previous analysis indicated a significant time delay, with a most likely value of 3.4 Gyr, effectively ruling out all previously proposed progenitor models, our analysis shows that the time-delay estimate is dominated by systematic errors, in particular due to...
Source: http://arxiv.org/abs/astro-ph/0601454v2
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47
Sep 24, 2013
09/13
by
F. Zhang; L. Li; Y. Zhang; X. Kang; Z. Han
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eye 47
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Using the evolutionary population synthesis (EPS) models with and without binary interactions (BIs), we present L_Ha, L_[OII], L_{i,UV} and L_FIR for Burst, S0, Sa-Sd and Irr galaxies, and present the calibrations of star formation rate (SFR) in terms of these diagnostics. By comparison, we find that BIs lower the SFR.vs.L_Ha and SFR.vs.L_[OII] conversion factors by ~0.2 dex. Moreover, BIs do not significantly vary the calibrations of SFR in terms of L_{i,UV}. In addition, BIs have little...
Source: http://arxiv.org/abs/1112.1165v2
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36
Sep 22, 2013
09/13
by
Z. Han; Ph. Podsiadlowski
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eye 36
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In this talk, we present the general principles of binary evolution and give two examples. The first example is the formation of subdwarf B stars (sdBs) and their application to the long-standing problem of ultraviolet excess (also known as UV-upturn) in elliptical galaxies. The second is for the progenitors of type Ia supernovae (SNe Ia). We discuss the main binary interactions, i.e., stable Roche lobe overflow (RLOF) and common envelope (CE) evolution, and show evolutionary channels leading...
Source: http://arxiv.org/abs/0805.3534v1
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56
Sep 18, 2013
09/13
by
Z. Han; Ph. Podsiadlowski; A. E. Lynas-Gray
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eye 56
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The discovery of a flux excess in the far-ultraviolet (UV) spectrum of elliptical galaxies was a major surprise in 1969. While it is now clear that this UV excess is caused by an old population of hot helium-burning stars without large hydrogen-rich envelopes, rather than young stars, their origin has remained a mystery. Here we show that these stars most likely lost their envelopes because of binary interactions, similar to the hot subdwarf population in our own Galaxy. We have developed an...
Source: http://arxiv.org/abs/0704.0863v3
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45
Sep 21, 2013
09/13
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Z. H. Zhang; H. R. A. Jones; D. J. Pinfield; R. S. Pokorny; Z. Han
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We selected brown dwarf candidates from the seventh Data Release of the Sloan Digital Sky Survey (SDSS DR7) with new photometric selectioncriteria based on a parameteriaztion of well-known L and T dwarfs. Then we confirmed their status with SDSS spectra. The candidates without SDSS spectra are cross matched in the Two Micron All Sky Survey (2MASS) and the Fourth Data Release of the UKIRT Infrared Deep Sky Survey (UKIDSS DR4). With the help of colors based on SDSS, 2MASS and UKIDSS, we are able...
Source: http://arxiv.org/abs/0902.2677v2
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3.0
Jun 30, 2018
06/18
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P. Leszczynski; Z. Han; A. A. L. Nicolet; B. A. Piot; P. Kossacki; M. Orlita; V. Bouchiat; D. M. Basko; M. Potemski; C. Faugeras
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We report a comprehensive study of the tuning with electric fields of the resonant magneto-exciton optical phonon coupling in gated graphene. For magnetic fields around $B \sim 25$ T which correspond to the range of the fundamental magneto-phonon resonance, the electron-phonon coupling can be switched on and off by tuning the position of the Fermi level in order to Pauli block the two fundamental inter Landau level excitations. The effects of such a profound change in the electronic excitation...
Topics: Mesoscale and Nanoscale Physics, Condensed Matter
Source: http://arxiv.org/abs/1402.0662
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44
Sep 23, 2013
09/13
by
X. Meng; X. Chen; Z. Han
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eye 44
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Following Paczy\'{n}ski & Zi\'{o}lkowski (1968) and Han et al. (1994), we assume that the envelope of an asymptotic giant branch (AGB) or a first giant branch (FGB) star is lost when the binding energy of the envelope is equal to zero ($\Delta W=0$) and the core mass of the AGB star or the FGB star at the point ($\Delta W=0$) is taken as the final mass. Using this assumption, we calculate the IFMRs for stars of different metallicities.We find that the IFMRs depends strongly on the...
Source: http://arxiv.org/abs/0710.2397v3
