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Shen, C. P.; Yuan, C. Z.; Wang, P.; Abdesselam, A.; Adachi, I.; Aihara, H.; Said, S. Al; Asner, D. M.; Aulchenko, V.; Aushev, T.; Ayad, R.; Bakich, A. M.; Bala, A.; Bobrov, A.; Bonvicini, G.; Bożek, A.; Bračko, M.; Browder, T. E.; Chekelian, V.; Chen, A.; Cheon, B. G.; Chilikin, K.; Chistov, R.; Cho, K.; Chobanova, V.; Choi, S. K.; Choi, Y.; Cinabro, D.; Dalseno, J.; Danilov, M.; Doležal, Z.; Drutskoy, A.; Dutta, D.; Eidelman, S.; Epifanov, D.; Farhat, H.; Fast, J. E.; Ferber, T.; Frey, A.; Gaur, V.; Ganguly, S.; Gillard, R.; Glattauer, R.; Goh, Y. M.; Golob, B.; Haba, J.; Hayasaka, K.; Hayashii, H.; He, X.; Hoshi, Y.; Hou, W.-S.; Hsiung, Y.; Hyun, H. J.; Iijima, T.; Ishikawa, A.; Itoh, R.; Iwasaki, Y.; Joffe, D.; Julius, T.; Kang, J. H.; Kato, E.; Kawasaki, T.; Kiesling, C.; Kim, D. Y.; Kim, H. J.; Kim, J. B.; Kim, J. H.; Kim, K. T.; Kim, M. J.; Kim, Y. J.; Kinoshita, K.; Ko, B. R.; Kodyš, P.; Korpar, S.; Križan, P.; Krokovny, P.; Kuzmin, A.; Kwon, Y. J.; Lee, Soohyung; Li, J.; Gioi, L. Li; Libby, J.; Liu, C.; Liu, Z. Q.; Lukin, P.; Matvienko, D.; Miyabayashi, K.; Miyata, H.; Mizuk, R.; Moll, A.; Mussa, R.; Nagasaka, Y.; Nakano, E.; Nakao, M.; Natkaniec, Z.; Nayak, M.; Nedelkovska, E.; Nisar, N. K.; Nishida, S.; Nitoh, O.; Okuno, S.; Park, C. W.; Park, H.; Pedlar, T. K.; Pestotnik, R.; Petrič, M.; Piilonen, L. E.; Ritter, M.; Röhrken, M.; Rostomyan, A.; Ryu, S.; Saito, T.; Sakai, Y.; Sanuki, T.; Sato, Y.; Schneider, O.; Schnell, G.; Semmler, D.; Senyo, K.; Seon, O.; Sevior, M. E.; Shapkin, M.; Shebalin, V.; Shibata, T. A.; Shiu, J. G.; Shwartz, B.; Sibidanov, A.; Simon, F.; Sohn, Y. S.; Sokolov, A.; Solovieva, E.; Stanič, S.; Starič, M.; Steder, M.; Sumiyoshi, T.; Tamponi, U.; Tatishvili, G.; Teramoto, Y.; Uchida, M.; Unno, Y.; Uno, S.; Urquijo, P.; Usov, Y.; Hulse, C. Van; Vanhoefer, P.; Varner, G.; Vorobyev, V.; Wagner, M. N.; Wang, C. H.; Watanabe, M.; Watanabe, Y.; Williams, K. M.; Won, E.; Yamamoto, H.; Yamashita, Y.; Yashchenko, S.; Yook, Y.; Zhang, C. C.; Zhang, Z. P.; Zhulanov, V.; Zupanc, A.

doi:10.1103/physrevd.89.072015

Cited by 48 publications

(22 citation statements)

References 44 publications

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“…Since 2011 the Belle Collaboration has produced a couple of initial-state radiation studies, involving production of J/ψK + K − and J/ψK S K S [29]; and ψ(2S)π + π − [30]. The focus of this work has been the search for resonant substructures in the final states.…”

Section: Belle At Kek-bmentioning

confidence: 99%

Radiative return capabilities of a high-energy, high-luminositye+e−collider

et al. 2015

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An electron-positron collider operating at a center-of-mass energy E CM can collect events at all lower energies through initial-state radiation (ISR or radiative return). We explore the capabilities for radiative return studies by a proposed high-luminosity collider at E CM = 250 or 90 GeV, to fill in gaps left by lowerenergy colliders such as PEP, PETRA, TRISTAN, and LEP. These capabilities are compared with those of the lower-energy e + e − colliders as well as hadron colliders such as the Tevatron and the CERN Large Hadron Collider (LHC). Some examples of accessible questions in dark photon searches and heavy flavor spectroscopy are given.PACS codes: 13.66.Bc, 13.66.De, 13.66.Hk I IntroductionAn electron-positron collider operating at a center-of-mass energy E CM can collect events at all lower energies through initial-state radiation (ISR). This radiative return process has been used to good advantage in e + e − colliders such as DAΦNE, PEP-II, KEK-B, and LEP [1][2][3][4]. In the present paper we explore the capabilities of a higher-energy high-luminosity e + e − collider such as that envisioned by CERN (FCC-ee) [5] or China (CEPC) [6], operating at E CM ≃ 250 or 90 GeV (functioning as a Giga-or Tera-Z factory at the latter energy) [7], to perform radiative return studies of physics at lower center-of-mass energies.In order to fairly assess the capabilities of future colliders with past and present colliders it is necessary to specify the total integrated luminosity expected to be collected by future †

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Section: Belle At Kek-bmentioning

confidence: 99%

Radiative return capabilities of a high-energy, high-luminositye+e−collider

et al. 2015

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“…Nevertheless, I keep the polytropic index as a free variable since it can vary in other situations. For example, if the WD was ignited from a detonating helium shell, the layer may have a convective profile instead (Bildsten et al 2007;Shen & Bildsten 2009;Woosley & Kasen 2011;Shen et al 2011).…”

Section: Dynamics and Thermodynamics Of Thementioning

confidence: 99%

RADIOACTIVELY POWERED RISING LIGHT CURVES OF TYPE Ia SUPERNOVAE

Piro

2012

ApJ

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The rising luminosity of the recent, nearby supernova 2011fe shows a quadratic dependence with time during the first ≈ 0.5 − 4 days. In addition, the composite lightcurves formed from stacking together many Type Ia supernovae (SNe Ia) show a similar power-law index of 1.8 ± 0.2 with time. I explore what range of power-law rises are possible due to the presence of radioactive material near the surface of the exploding white dwarf (WD). I summarize what constraints such a model places on the structure of the progenitor and the distribution and velocity of ejecta. My main conclusion is that the rise of SN 2011fe requires a mass fraction X 56 ≈ 3 × 10 −2 of 56 Ni (or some other heating source like 48 Cr) distributed between a depth of ≈ 4 × 10 −3 − 0.1M ⊙ below the WD's surface. Radioactive elements this shallow are not found in simulations of a single C/O detonation. Scenarios that may produce this material include helium-shell burning during a double-detonation ignition, a gravitationally confined detonation, and a subset of deflagration to detonation transition models. In general, the power-law rise can differ from quadratic depending on the details of the event, so comparisons of this work with observed bolometric rises of SNe Ia would place strong constraints on the distribution of shallow radioactive material, providing important clues for identifying the elusive progenitors of SNe Ia.

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“…at and/or above their common threshold at 4.43 GeV. The available data of a study using initial state radiation at Belle[48] indicate a certain activity in the final state J/ψKK above 4.4 GeV with possible structures. However more detailed data on the yield of strange Ds mesons and/or of J/ψKK in that energy range are needed for further conclusions.…”

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confidence: 97%

Bottomonium-like states: Physics case for energy scan above the BB̄ threshold at Belle-II

2017

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The Belle-II experiment is expected to collect large data samples at the Υ(4S) and Υ(5S) resonances to study primarily B and Bs mesons. We discuss what other data above the BB threshold are of interest. We propose to perform a high-statistics energy scan from the BB threshold up to the highest possible energy, and to collect data at the Υ(6S) and at higher mass states if they are found in the scan. We emphasize the interest in increasing the maximal energy from 11.24 GeV to 11.5 − 12 GeV in the future. These data are needed for investigation of bottomonium and bottomonium-like states.

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Updated cross section measurement ofe+e−→K+K

Cited by 48 publications

References 44 publications

Radiative return capabilities of a high-energy, high-luminositye+e−collider

Radiative return capabilities of a high-energy, high-luminositye+e−collider

RADIOACTIVELY POWERED RISING LIGHT CURVES OF TYPE Ia SUPERNOVAE

Bottomonium-like states: Physics case for energy scan above the BB̄ threshold at Belle-II

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