Focus on:
All days
Mar 3, 2020
Mar 4, 2020
Mar 5, 2020
Mar 6, 2020
All sessions
Dinner (Cafeteria AZAMI, on campus)
Discussion on the Universe
Opening
Poster session (Hall of the Student Union building)
Registration
Summary, Closing
Tour of the Gravitational Wave Research Laboratory
Hide Contributions
Compact style
Indico style
Indico style - inline minutes
Indico style - numbered
Indico style - numbered + minutes
Indico Weeks View
Back to Conference View
Choose Timezone
Use the event/category timezone
Specify a timezone
Africa/Abidjan
Africa/Accra
Africa/Addis_Ababa
Africa/Algiers
Africa/Asmara
Africa/Bamako
Africa/Bangui
Africa/Banjul
Africa/Bissau
Africa/Blantyre
Africa/Brazzaville
Africa/Bujumbura
Africa/Cairo
Africa/Casablanca
Africa/Ceuta
Africa/Conakry
Africa/Dakar
Africa/Dar_es_Salaam
Africa/Djibouti
Africa/Douala
Africa/El_Aaiun
Africa/Freetown
Africa/Gaborone
Africa/Harare
Africa/Johannesburg
Africa/Juba
Africa/Kampala
Africa/Khartoum
Africa/Kigali
Africa/Kinshasa
Africa/Lagos
Africa/Libreville
Africa/Lome
Africa/Luanda
Africa/Lubumbashi
Africa/Lusaka
Africa/Malabo
Africa/Maputo
Africa/Maseru
Africa/Mbabane
Africa/Mogadishu
Africa/Monrovia
Africa/Nairobi
Africa/Ndjamena
Africa/Niamey
Africa/Nouakchott
Africa/Ouagadougou
Africa/Porto-Novo
Africa/Sao_Tome
Africa/Tripoli
Africa/Tunis
Africa/Windhoek
America/Adak
America/Anchorage
America/Anguilla
America/Antigua
America/Araguaina
America/Argentina/Buenos_Aires
America/Argentina/Catamarca
America/Argentina/Cordoba
America/Argentina/Jujuy
America/Argentina/La_Rioja
America/Argentina/Mendoza
America/Argentina/Rio_Gallegos
America/Argentina/Salta
America/Argentina/San_Juan
America/Argentina/San_Luis
America/Argentina/Tucuman
America/Argentina/Ushuaia
America/Aruba
America/Asuncion
America/Atikokan
America/Bahia
America/Bahia_Banderas
America/Barbados
America/Belem
America/Belize
America/Blanc-Sablon
America/Boa_Vista
America/Bogota
America/Boise
America/Cambridge_Bay
America/Campo_Grande
America/Cancun
America/Caracas
America/Cayenne
America/Cayman
America/Chicago
America/Chihuahua
America/Costa_Rica
America/Creston
America/Cuiaba
America/Curacao
America/Danmarkshavn
America/Dawson
America/Dawson_Creek
America/Denver
America/Detroit
America/Dominica
America/Edmonton
America/Eirunepe
America/El_Salvador
America/Fort_Nelson
America/Fortaleza
America/Glace_Bay
America/Goose_Bay
America/Grand_Turk
America/Grenada
America/Guadeloupe
America/Guatemala
America/Guayaquil
America/Guyana
America/Halifax
America/Havana
America/Hermosillo
America/Indiana/Indianapolis
America/Indiana/Knox
America/Indiana/Marengo
America/Indiana/Petersburg
America/Indiana/Tell_City
America/Indiana/Vevay
America/Indiana/Vincennes
America/Indiana/Winamac
America/Inuvik
America/Iqaluit
America/Jamaica
America/Juneau
America/Kentucky/Louisville
America/Kentucky/Monticello
America/Kralendijk
America/La_Paz
America/Lima
America/Los_Angeles
America/Lower_Princes
America/Maceio
America/Managua
America/Manaus
America/Marigot
America/Martinique
America/Matamoros
America/Mazatlan
America/Menominee
America/Merida
America/Metlakatla
America/Mexico_City
America/Miquelon
America/Moncton
America/Monterrey
America/Montevideo
America/Montserrat
America/Nassau
America/New_York
America/Nome
America/Noronha
America/North_Dakota/Beulah
America/North_Dakota/Center
America/North_Dakota/New_Salem
America/Nuuk
America/Ojinaga
America/Panama
America/Pangnirtung
America/Paramaribo
America/Phoenix
America/Port-au-Prince
America/Port_of_Spain
America/Porto_Velho
America/Puerto_Rico
America/Punta_Arenas
America/Rankin_Inlet
America/Recife
America/Regina
America/Resolute
America/Rio_Branco
America/Santarem
America/Santiago
America/Santo_Domingo
America/Sao_Paulo
America/Scoresbysund
America/Sitka
America/St_Barthelemy
America/St_Johns
America/St_Kitts
America/St_Lucia
America/St_Thomas
America/St_Vincent
America/Swift_Current
America/Tegucigalpa
America/Thule
America/Tijuana
America/Toronto
America/Tortola
America/Vancouver
America/Whitehorse
America/Winnipeg
America/Yakutat
America/Yellowknife
Antarctica/Casey
Antarctica/Davis
Antarctica/DumontDUrville
Antarctica/Macquarie
Antarctica/Mawson
Antarctica/McMurdo
Antarctica/Palmer
Antarctica/Rothera
Antarctica/Syowa
Antarctica/Troll
Antarctica/Vostok
Arctic/Longyearbyen
Asia/Aden
Asia/Almaty
Asia/Amman
Asia/Anadyr
Asia/Aqtau
Asia/Aqtobe
Asia/Ashgabat
Asia/Atyrau
Asia/Baghdad
Asia/Bahrain
Asia/Baku
Asia/Bangkok
Asia/Barnaul
Asia/Beirut
Asia/Bishkek
Asia/Brunei
Asia/Chita
Asia/Choibalsan
Asia/Colombo
Asia/Damascus
Asia/Dhaka
Asia/Dili
Asia/Dubai
Asia/Dushanbe
Asia/Famagusta
Asia/Gaza
Asia/Hebron
Asia/Ho_Chi_Minh
Asia/Hong_Kong
Asia/Hovd
Asia/Irkutsk
Asia/Jakarta
Asia/Jayapura
Asia/Jerusalem
Asia/Kabul
Asia/Kamchatka
Asia/Karachi
Asia/Kathmandu
Asia/Khandyga
Asia/Kolkata
Asia/Krasnoyarsk
Asia/Kuala_Lumpur
Asia/Kuching
Asia/Kuwait
Asia/Macau
Asia/Magadan
Asia/Makassar
Asia/Manila
Asia/Muscat
Asia/Nicosia
Asia/Novokuznetsk
Asia/Novosibirsk
Asia/Omsk
Asia/Oral
Asia/Phnom_Penh
Asia/Pontianak
Asia/Pyongyang
Asia/Qatar
Asia/Qostanay
Asia/Qyzylorda
Asia/Riyadh
Asia/Sakhalin
Asia/Samarkand
Asia/Seoul
Asia/Shanghai
Asia/Singapore
Asia/Srednekolymsk
Asia/Taipei
Asia/Tashkent
Asia/Tbilisi
Asia/Tehran
Asia/Thimphu
Asia/Tokyo
Asia/Tomsk
Asia/Ulaanbaatar
Asia/Urumqi
Asia/Ust-Nera
Asia/Vientiane
Asia/Vladivostok
Asia/Yakutsk
Asia/Yangon
Asia/Yekaterinburg
Asia/Yerevan
Atlantic/Azores
Atlantic/Bermuda
Atlantic/Canary
Atlantic/Cape_Verde
Atlantic/Faroe
Atlantic/Madeira
Atlantic/Reykjavik
Atlantic/South_Georgia
Atlantic/St_Helena
Atlantic/Stanley
Australia/Adelaide
Australia/Brisbane
Australia/Broken_Hill
Australia/Darwin
Australia/Eucla
Australia/Hobart
Australia/Lindeman
Australia/Lord_Howe
Australia/Melbourne
Australia/Perth
Australia/Sydney
Canada/Atlantic
Canada/Central
Canada/Eastern
Canada/Mountain
Canada/Newfoundland
Canada/Pacific
Europe/Amsterdam
Europe/Andorra
Europe/Astrakhan
Europe/Athens
Europe/Belgrade
Europe/Berlin
Europe/Bratislava
Europe/Brussels
Europe/Bucharest
Europe/Budapest
Europe/Busingen
Europe/Chisinau
Europe/Copenhagen
Europe/Dublin
Europe/Gibraltar
Europe/Guernsey
Europe/Helsinki
Europe/Isle_of_Man
Europe/Istanbul
Europe/Jersey
Europe/Kaliningrad
Europe/Kirov
Europe/Kyiv
Europe/Lisbon
Europe/Ljubljana
Europe/London
Europe/Luxembourg
Europe/Madrid
Europe/Malta
Europe/Mariehamn
Europe/Minsk
Europe/Monaco
Europe/Moscow
Europe/Oslo
Europe/Paris
Europe/Podgorica
Europe/Prague
Europe/Riga
Europe/Rome
Europe/Samara
Europe/San_Marino
Europe/Sarajevo
Europe/Saratov
Europe/Simferopol
Europe/Skopje
Europe/Sofia
Europe/Stockholm
Europe/Tallinn
Europe/Tirane
Europe/Ulyanovsk
Europe/Vaduz
Europe/Vatican
Europe/Vienna
Europe/Vilnius
Europe/Volgograd
Europe/Warsaw
Europe/Zagreb
Europe/Zurich
GMT
Indian/Antananarivo
Indian/Chagos
Indian/Christmas
Indian/Cocos
Indian/Comoro
Indian/Kerguelen
Indian/Mahe
Indian/Maldives
Indian/Mauritius
Indian/Mayotte
Indian/Reunion
Pacific/Apia
Pacific/Auckland
Pacific/Bougainville
Pacific/Chatham
Pacific/Chuuk
Pacific/Easter
Pacific/Efate
Pacific/Fakaofo
Pacific/Fiji
Pacific/Funafuti
Pacific/Galapagos
Pacific/Gambier
Pacific/Guadalcanal
Pacific/Guam
Pacific/Honolulu
Pacific/Kanton
Pacific/Kiritimati
Pacific/Kosrae
Pacific/Kwajalein
Pacific/Majuro
Pacific/Marquesas
Pacific/Midway
Pacific/Nauru
Pacific/Niue
Pacific/Norfolk
Pacific/Noumea
Pacific/Pago_Pago
Pacific/Palau
Pacific/Pitcairn
Pacific/Pohnpei
Pacific/Port_Moresby
Pacific/Rarotonga
Pacific/Saipan
Pacific/Tahiti
Pacific/Tarawa
Pacific/Tongatapu
Pacific/Wake
Pacific/Wallis
US/Alaska
US/Arizona
US/Central
US/Eastern
US/Hawaii
US/Mountain
US/Pacific
UTC
Save
Asia/Tokyo
English (United States)
Deutsch (Deutschland)
English (United Kingdom)
English (United States)
Español (España)
Français (France)
Polski (Polska)
Português (Brasil)
Türkçe (Türkiye)
Монгол (Монгол)
Українська (Україна)
中文 (中国)
Login
The 2nd Toyama International Symposium on "Physics at the Cosmic Frontier" (PCF2020)
from
Tuesday, March 3, 2020 (9:00 AM)
to
Friday, March 6, 2020 (6:00 PM)
Monday, March 2, 2020
Tuesday, March 3, 2020
10:00 AM
10:00 AM - 10:30 AM
Room: A238
10:30 AM
10:30 AM - 10:50 AM
Room: A238
10:50 AM
KAGRA status
-
Matteo Leonardi
(
NAOJ
)
KAGRA status
Matteo Leonardi
(
NAOJ
)
10:50 AM - 11:30 AM
Room: A238
After the first detection of gravitational waves coming from a binary blackhole merger in 2015, the field of gravitational wave astronomy has started. Nowadays, the second generation gravitational wave detectors LIGO (in the US) and Virgo (in Italy) have improved their sensitivity substantially with respect of the time of the first detection, increasing the detection volume of about one order of magnitude. Such improvement led to the current detection rate of one event per week, on average. In Japan, KAGRA, the first 2.5G detector, has been built and has started a commissioning phase which will lead to a joint observation run with LIGO and Virgo detectors. KAGRA has two unique features: it is located in an underground facility and has cryogenic mirrors. The first feature will allow for a reduction of the seismic and newtonian noises, which are currently limiting the low frequency region of LIGO and Virgo. The second one will help to reduce the impact of the thermal or brownian noise which is a huge limitation in the central and most sensitive frequency region of gravitational wave detectors.
11:30 AM
Model experiment of cosmic ray acceleration
-
Yasuhiro Kuramitsu
(
Osaka University
)
Model experiment of cosmic ray acceleration
Yasuhiro Kuramitsu
(
Osaka University
)
11:30 AM - 12:10 PM
Room: A238
12:10 PM
Lunch
Lunch
12:10 PM - 1:30 PM
Room: Cafeteria
1:30 PM
Turbulent dynamos
-
Nobumitsu Yokoi
(
University of Tokyo
)
Turbulent dynamos
Nobumitsu Yokoi
(
University of Tokyo
)
1:30 PM - 2:10 PM
Room: A238
In the presence of symmetry breakage, turbulence may contribute to suppression of effective transport, counter-balancing its primary effect: enhancement of transport. This dynamic balance leads to a large-scale structure formation: turbulent dynamos. In this talk, firstly, an attempt to theoretically tackle strongly nonlinear and inhomogeneous turbulence is presented. Then, the theoretical results are used for constructing a self-consistent turbulent dynamo model beyond the conventional heuristic ad hoc modelling approaches. Finally, astrophysical applications of a dynamo model in strongly compressible magnetohydrodynamic turbulence will be discussed.
2:10 PM
Spontaneous structure formation of aurora due to magnetosphere-ionosphere coupling
-
Seiya Nishimura
(
Hosei University
)
Spontaneous structure formation of aurora due to magnetosphere-ionosphere coupling
Seiya Nishimura
(
Hosei University
)
2:10 PM - 2:50 PM
Room: A238
Feedback instability occurs in a coupling system of the magnetosphere and the ionosphere, and is a theoretical model explaining spontaneous development of the quiet aurora. In this study, we extend a model of the magnetosphere in the feedback instability to the gyrofluid model. This extension makes it possible to properly discuss kinetic effects, such as the finite Larmor radius effect, the Landau damping, and the mirror force, on the feedback instability in a framework of a fluid model. The derived model is applied to linear stability analysis and nonlinear simulation of the feedback instability.
2:50 PM
Break
Break
2:50 PM - 3:20 PM
Room: A238
3:20 PM
Non-equilibrium dynamics in warm dense matter by Free Electron Laser radiation
-
Keisuke Hatada
(
University of Toyama
)
Non-equilibrium dynamics in warm dense matter by Free Electron Laser radiation
Keisuke Hatada
(
University of Toyama
)
3:20 PM - 4:00 PM
Room: A238
4:00 PM
Development of Auxiliary Locking System in Gravitational Wave Telescope KAGRA
-
Ryosuke Sugimoto
(
University of Toyama
)
Development of Auxiliary Locking System in Gravitational Wave Telescope KAGRA
Ryosuke Sugimoto
(
University of Toyama
)
4:00 PM - 4:20 PM
Room: A238
Development of Auxiliary Locking System in Gravitational Wave Telescope KAGRA I'll modify it later.
4:20 PM
Current status of intensity stabilitzation system in KAGRA
-
Kanta Yamashita
(
University of Toyama
)
Current status of intensity stabilitzation system in KAGRA
Kanta Yamashita
(
University of Toyama
)
4:20 PM - 4:40 PM
Room: A238
I will fix it later.
4:40 PM
Break
Break
4:40 PM - 5:10 PM
Room: A238
5:10 PM
5:10 PM - 5:50 PM
Room: GW Research Lab
Wednesday, March 4, 2020
9:00 AM
General-relativistic magnetohydrodynamics
-
Akira Mizuta
(
RIKEN
)
General-relativistic magnetohydrodynamics
Akira Mizuta
(
RIKEN
)
9:00 AM - 9:40 AM
Room: A238
9:40 AM
Chiral magnetohydrodynamics in cosmology
-
Tomohiro Fujita
(
Kyoto University
)
Chiral magnetohydrodynamics in cosmology
Tomohiro Fujita
(
Kyoto University
)
9:40 AM - 10:20 AM
Room: A238
10:20 AM
Photo + Break
Photo + Break
10:20 AM - 10:50 AM
Room: A238
10:50 AM
Beyond the Standard Model of particle physics
-
Mayumi Aoki
(
Kanazawa University
)
Beyond the Standard Model of particle physics
Mayumi Aoki
(
Kanazawa University
)
10:50 AM - 11:30 AM
Room: A238
11:30 AM
Collider physics
-
Kentarou Mawatari
(
Osaka U.
)
Collider physics
Kentarou Mawatari
(
Osaka U.
)
11:30 AM - 12:10 PM
Room: A238
12:10 PM
Lunch
Lunch
12:10 PM - 1:30 PM
Room: Cafeteria
1:30 PM
1:30 PM - 5:30 PM
Room: A238
Thursday, March 5, 2020
9:00 AM
Gravitational wave turbulence in the early Universe
-
Sébastien Galtier
(
France
)
Gravitational wave turbulence in the early Universe
Sébastien Galtier
(
France
)
9:00 AM - 9:40 AM
Room: A238
The non-linear nature of the general relativity equations suggests that space-time can be turbulent. Such a turbulence may happen in the primordial universe (first second). The analytical theory of weak gravitational wave (GW) turbulence [1] was built from a diagonal space-time metric reduced to the variables t, x and y [2]. The theory predicts the existence of a dual cascade driven by 4–wave interactions with a direct cascade of energy and an inverse cascade of wave action. In the latter case the wave action spectrum - an exact solution of the equations - has the power law index -2/3 involving an explosive phenomenon. In this context, we developed a nonlinear diffusion model in spectral space to describe GW turbulence in the approximation of strongly local interactions [3]. We showed analytically that the model equation satisfies the conservation of energy and wave action, and reproduces the power law solutions previously derived from the kinetic equations. We showed numerically that in the non-stationary regime the wave action spectrum presents an anomalous scaling which is understood as a self-similar solution of the second kind. The regime of weak GW turbulence is actually limited to a narrow wavenumber window and turbulence is expected to become strong at larger scales. Then the phenomenology of critical balance can be used. The formation of a condensate may happen and its rapid growth can be interpreted as an accelerated expansion of the universe that could be at the origin of the cosmic inflation. We can show with this scenario that the fossil spectrum obtained after inflation is compatible with the latest data obtained with the Planck/ESA satellite [4]. [1] Galtier & Nazarenko, Phys. Rev. Lett. **119**, 221101 (2017) [2] Hadad & Zakharov, J. Geom. Phys. **80**, 37 (2014) [3] Galtier, Nazarenko, Buchlin & Thalabard, Physica D **390**, 84 (2019) [4] Galtier, Nazarenko & Laurie (2020)
9:40 AM
Laser produced-plasmas
-
Shuta Tanaka
(
Aoyama Gakuin Universuty
)
Laser produced-plasmas
Shuta Tanaka
(
Aoyama Gakuin Universuty
)
9:40 AM - 10:20 AM
Room: A238
10:20 AM
Break
Break
10:20 AM - 10:50 AM
Room: A238
10:50 AM
Dark matter interpretation of CALET data
-
Holger Martin Motz
(
Waseda University
)
Dark matter interpretation of CALET data
Holger Martin Motz
(
Waseda University
)
10:50 AM - 11:30 AM
Room: A238
11:30 AM
Introduction to Neutrino Physics
-
Hiroaki Sugiyama
Introduction to Neutrino Physics
Hiroaki Sugiyama
11:30 AM - 12:10 PM
Room: A238
I introduce basics on neutrino physics
12:10 PM
Lunch
Lunch
12:10 PM - 1:40 PM
Room: A238
1:40 PM
Modeling evolution of dark matter substructure and annihilation boost
-
Nagisa Hiroshima
Modeling evolution of dark matter substructure and annihilation boost
Nagisa Hiroshima
1:40 PM - 2:20 PM
Room: A238
The structure of dark matter halo is hierarchical. Among them, small-scale structures in dark matter halo, (so-called subhalos,) can enhance dark matter annihilation signals. It is necessary to quantify boost factors by those subhalos to derive the property of dark matter with current/future gamma-ray observations. In order to derive the subhalo boost factors, calculations of halo structure covering more than 20 orders-of-magnitude in the halo mass up to a redshift of ~10 are required. This is beyond the capability of the current state-of-art cosmological N-body simulation which is a widely-adopted method to study the halo structure. In this talk, I introduce our analytical approach for the formalism of subhalo evolutions and the resultant boost factors. I show that the constraints on the annihilation cross-section obtained by isotropic gamma-ray observations can be updated by several factors by taking the contribution from subhalos into account.
2:20 PM
MeV-scale reheating temperature and cosmological constraints on sterile neutrinos
-
Takuya Hasegawa
(
KEK
)
MeV-scale reheating temperature and cosmological constraints on sterile neutrinos
Takuya Hasegawa
(
KEK
)
2:20 PM - 2:40 PM
Room: A238
In this study, we investigate a possible existence of sterile neutrinos with a various range of masses in terms of cosmology assuming an MeV-scale reheating temperature. By numerically calculating sterile neutrino production through flavor mixing, we find that the existence of light sterile neutrinos inferred from short-baseline neutrino oscillation experiments becomes consistent with observational results of big-bang nucleosynthesis (BBN) for the reheating temperature of O(1) MeV if the scalar particle responsible for the reheating fully decay into radiations. In contrast, if the scalar particle mainly decays into hadrons, the BBN bound becomes more stringent, and the allowed region for the light sterile neutrino is completely excluded, depending on the mass of the scalar particle and the hadronic branching ratio of the decay.
2:40 PM
Testing Gauge-Higgs Unification Models by Measuring the Triple Higgs Boson Coupling at Future Collider Experiments
-
Shin Suzuki
(
University of Toyama
)
Testing Gauge-Higgs Unification Models by Measuring the Triple Higgs Boson Coupling at Future Collider Experiments
Shin Suzuki
(
University of Toyama
)
2:40 PM - 3:00 PM
Room: A238
Gauge-Higgs Unification is a TeV-scale paradigm solving the hierarchy problem. It has a characteristic Higgs potential induced by quantum corrections. In this work, as a realistic gauge-Higgs unification model we consider a SU(3) model with 5-dimensional Lorentz symmetry relaxed. And we consider the testability of this model by measuring the triple Higgs boson coupling at future collider experiments, such as the HL-LHC and ILC.
3:00 PM
Break
Break
3:00 PM - 3:30 PM
Room: A238
3:30 PM
Robustness of particle creation in a formation of a compact object
-
Okabayashi Kazumasa
(
Osaka City University
)
Robustness of particle creation in a formation of a compact object
Okabayashi Kazumasa
(
Osaka City University
)
3:30 PM - 3:50 PM
Room: A238
The fact that particle creation arises even in a formation of compact horizonless object has been applied to distinguish between a black hole and a black hole mimic. In this approach, it is revealed that radiation from a compact object is mainly classified into three types: transient Hawking radiation, post-Hawking burst, and late-time burst. However, these models are using a hollow shell and not realistic. Thus, we evaluate particle creation in a concrete model having matter at first. Interestingly, similar results to the case for the hollow shell model is obtained. This implies that particle creation in a formation of a compact object has robust property. Hence, we explore how common property this robustness is in a more general shell model. In order to explore this robustness, we assume conditions between the outside and inside null coordinates of the shell and show that particle creation in a formation of a compact object is robustness in the sense that radiation power does not depend on the inside detail.
3:50 PM
Theoretical study of Photoelectron Angular Distributions for Dicationic Carbon Monoxide by the use of Full-Potential Multiple Scattering Theory
-
Fukiko Ohta
(
University of Toyama
)
Theoretical study of Photoelectron Angular Distributions for Dicationic Carbon Monoxide by the use of Full-Potential Multiple Scattering Theory
Fukiko Ohta
(
University of Toyama
)
3:50 PM - 4:10 PM
Room: A238
4:10 PM
Challenges for MCMS (Multi-Channel Multiple Scattering) theory in solid state
-
Aika Takatsu
Challenges for MCMS (Multi-Channel Multiple Scattering) theory in solid state
Aika Takatsu
4:10 PM - 4:30 PM
Room: A238
Friday, March 6, 2020
9:00 AM
Machine learning for computational astrophysics
-
Yosuke Matsumoto
(
Chiba University
)
Machine learning for computational astrophysics
Yosuke Matsumoto
(
Chiba University
)
9:00 AM - 9:40 AM
Room: A238
We present our recent progress on implementing neural network's inference into magnetohydrodynamic simulations for astrophysical phenomena.
9:40 AM
Low-scale flavon model with a Z_N symmetry
-
Tetsutaro Higaki
(
Keio University
)
Low-scale flavon model with a Z_N symmetry
Tetsutaro Higaki
(
Keio University
)
9:40 AM - 10:20 AM
Room: A238
We propose a model that explains the fermion mass hierarchy by the Froggatt-Nielsen mechanism with a discrete Z_N flavor symmetry. As a concrete model, we study a supersymmetric model with a single flavon coupled to the minimal supersymmetric Standard Model. Flavon develops a TeV scale vacuum expectation value for realizing flavor hierarchy, an appropriate µ-term and the electroweak scale, hence the model has a low cutoff scale. We demonstrate how the flavon is successfully stabilized together with the Higgs bosons in the model. The discrete flavor symmetry Z_N controls not only the Standard Model fermion masses, but also the Higgs potential and a mass of the Higgsino which is a good candidate for dark matter. The hierarchy in the Higgs-flavon sector is determined in order to make the model anomaly-free and realize a stable electroweak vacuum. We show that this model can explain the fermion mass hierarchy, realistic Higgs-flavon potential and thermally produced dark matter at the same time. We discuss flavor violating processes induced by the light flavon which would be detected in future experiments.
10:20 AM
Break
Break
10:20 AM - 10:50 AM
Room: A238
10:50 AM
The Higgs sector and gravitational waves
-
Mitsuru Kakizaki
(
University of Toyama
)
The Higgs sector and gravitational waves
Mitsuru Kakizaki
(
University of Toyama
)
10:50 AM - 11:30 AM
Room: A238
I will talk about the Higgs sector and gravitational waves.
11:30 AM
11:30 AM - 12:00 PM
Room: A238