# D. ESPRIU

## Contact Details

NameD. ESPRIU |
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Affiliation |
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Location |
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## Pubs By Year |
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## Pub CategoriesHigh Energy Physics - Phenomenology (41) High Energy Physics - Theory (22) Nuclear Theory (12) General Relativity and Quantum Cosmology (10) Cosmology and Nongalactic Astrophysics (9) High Energy Astrophysical Phenomena (5) High Energy Physics - Experiment (4) Nuclear Experiment (3) Astrophysics (2) High Energy Physics - Lattice (2) Physics - Statistical Mechanics (1) Solar and Stellar Astrophysics (1) |

## Publications Authored By D. ESPRIU

**Authors:**D. de Florian

^{1}, C. Grojean

^{2}, F. Maltoni

^{3}, C. Mariotti

^{4}, A. Nikitenko

^{5}, M. Pieri

^{6}, P. Savard

^{7}, M. Schumacher

^{8}, R. Tanaka

^{9}, R. Aggleton

^{10}, M. Ahmad

^{11}, B. Allanach

^{12}, C. Anastasiou

^{13}, W. Astill

^{14}, S. Badger

^{15}, M. Badziak

^{16}, J. Baglio

^{17}, E. Bagnaschi

^{18}, A. Ballestrero

^{19}, A. Banfi

^{20}, D. Barducci

^{21}, M. Beckingham

^{22}, C. Becot

^{23}, G. Bélanger

^{24}, J. Bellm

^{25}, N. Belyaev

^{26}, F. U. Bernlochner

^{27}, C. Beskidt

^{28}, A. Biekötter

^{29}, F. Bishara

^{30}, W. Bizon

^{31}, N. E. Bomark

^{32}, M. Bonvini

^{33}, S. Borowka

^{34}, V. Bortolotto

^{35}, S. Boselli

^{36}, F. J. Botella

^{37}, R. Boughezal

^{38}, G. C. Branco

^{39}, J. Brehmer

^{40}, L. Brenner

^{41}, S. Bressler

^{42}, I. Brivio

^{43}, A. Broggio

^{44}, H. Brun

^{45}, G. Buchalla

^{46}, C. D. Burgard

^{47}, A. Calandri

^{48}, L. Caminada

^{49}, R. Caminal Armadans

^{50}, F. Campanario

^{51}, J. Campbell

^{52}, F. Caola

^{53}, C. M. Carloni Calame

^{54}, S. Carrazza

^{55}, A. Carvalho

^{56}, M. Casolino

^{57}, O. Cata

^{58}, A. Celis

^{59}, F. Cerutti

^{60}, N. Chanon

^{61}, M. Chen

^{62}, X. Chen

^{63}, B. Chokoufé Nejad

^{64}, N. Christensen

^{65}, M. Ciuchini

^{66}, R. Contino

^{67}, T. Corbett

^{68}, D. Curtin

^{69}, M. Dall'Osso

^{70}, A. David

^{71}, S. Dawson

^{72}, J. de Blas

^{73}, W. de Boer

^{74}, P. de Castro Manzano

^{75}, C. Degrande

^{76}, R. L. Delgado

^{77}, F. Demartin

^{78}, A. Denner

^{79}, B. Di Micco

^{80}, R. Di Nardo

^{81}, S. Dittmaier

^{82}, A. Dobado

^{83}, T. Dorigo

^{84}, F. A. Dreyer

^{85}, M. Dührssen

^{86}, C. Duhr

^{87}, F. Dulat

^{88}, K. Ecker

^{89}, K. Ellis

^{90}, U. Ellwanger

^{91}, C. Englert

^{92}, D. Espriu

^{93}, A. Falkowski

^{94}, L. Fayard

^{95}, R. Feger

^{96}, G. Ferrera

^{97}, A. Ferroglia

^{98}, N. Fidanza

^{99}, T. Figy

^{100}, M. Flechl

^{101}, D. Fontes

^{102}, S. Forte

^{103}, P. Francavilla

^{104}, E. Franco

^{105}, R. Frederix

^{106}, A. Freitas

^{107}, F. F. Freitas

^{108}, F. Frensch

^{109}, S. Frixione

^{110}, B. Fuks

^{111}, E. Furlan

^{112}, S. Gadatsch

^{113}, J. Gao

^{114}, Y. Gao

^{115}, M. V. Garzelli

^{116}, T. Gehrmann

^{117}, R. Gerosa

^{118}, M. Ghezzi

^{119}, D. Ghosh

^{120}, S. Gieseke

^{121}, D. Gillberg

^{122}, G. F. Giudice

^{123}, E. W. N. Glover

^{124}, F. Goertz

^{125}, D. Gonçalves

^{126}, J. Gonzalez-Fraile

^{127}, M. Gorbahn

^{128}, S. Gori

^{129}, C. A. Gottardo

^{130}, M. Gouzevitch

^{131}, P. Govoni

^{132}, D. Gray

^{133}, M. Grazzini

^{134}, N. Greiner

^{135}, A. Greljo

^{136}, J. Grigo

^{137}, A. V. Gritsan

^{138}, R. Gröber

^{139}, S. Guindon

^{140}, H. E. Haber

^{141}, C. Han

^{142}, T. Han

^{143}, R. Harlander

^{144}, M. A. Harrendorf

^{145}, H. B. Hartanto

^{146}, C. Hays

^{147}, S. Heinemeyer

^{148}, G. Heinrich

^{149}, M. Herrero

^{150}, F. Herzog

^{151}, B. Hespel

^{152}, V. Hirschi

^{153}, S. Hoeche

^{154}, S. Honeywell

^{155}, S. J. Huber

^{156}, C. Hugonie

^{157}, J. Huston

^{158}, A. Ilnicka

^{159}, G. Isidori

^{160}, B. Jäger

^{161}, M. Jaquier

^{162}, S. P. Jones

^{163}, A. Juste

^{164}, S. Kallweit

^{165}, A. Kaluza

^{166}, A. Kardos

^{167}, A. Karlberg

^{168}, Z. Kassabov

^{169}, N. Kauer

^{170}, D. I. Kazakov

^{171}, M. Kerner

^{172}, W. Kilian

^{173}, F. Kling

^{174}, K. Köneke

^{175}, R. Kogler

^{176}, R. Konoplich

^{177}, S. Kortner

^{178}, S. Kraml

^{179}, C. Krause

^{180}, F. Krauss

^{181}, M. Krawczyk

^{182}, A. Kulesza

^{183}, S. Kuttimalai

^{184}, R. Lane

^{185}, A. Lazopoulos

^{186}, G. Lee

^{187}, P. Lenzi

^{188}, I. M. Lewis

^{189}, Y. Li

^{190}, S. Liebler

^{191}, J. Lindert

^{192}, X. Liu

^{193}, Z. Liu

^{194}, F. J. Llanes-Estrada

^{195}, H. E. Logan

^{196}, D. Lopez-Val

^{197}, I. Low

^{198}, G. Luisoni

^{199}, P. Maierhöfer

^{200}, E. Maina

^{201}, B. Mansoulié

^{202}, H. Mantler

^{203}, M. Mantoani

^{204}, A. C. Marini

^{205}, V. I. Martinez Outschoorn

^{206}, S. Marzani

^{207}, D. Marzocca

^{208}, A. Massironi

^{209}, K. Mawatari

^{210}, J. Mazzitelli

^{211}, A. McCarn

^{212}, B. Mellado

^{213}, K. Melnikov

^{214}, S. B. Menari

^{215}, L. Merlo

^{216}, C. Meyer

^{217}, P. Milenovic

^{218}, K. Mimasu

^{219}, S. Mishima

^{220}, B. Mistlberger

^{221}, S. -O. Moch

^{222}, A. Mohammadi

^{223}, P. F. Monni

^{224}, G. Montagna

^{225}, M. Moreno Llácer

^{226}, N. Moretti

^{227}, S. Moretti

^{228}, L. Motyka

^{229}, A. Mück

^{230}, M. Mühlleitner

^{231}, S. Munir

^{232}, P. Musella

^{233}, P. Nadolsky

^{234}, D. Napoletano

^{235}, M. Nebot

^{236}, C. Neu

^{237}, M. Neubert

^{238}, R. Nevzorov

^{239}, O. Nicrosini

^{240}, J. Nielsen

^{241}, K. Nikolopoulos

^{242}, J. M. No

^{243}, C. O'Brien

^{244}, T. Ohl

^{245}, C. Oleari

^{246}, T. Orimoto

^{247}, D. Pagani

^{248}, C. E. Pandini

^{249}, A. Papaefstathiou

^{250}, A. S. Papanastasiou

^{251}, G. Passarino

^{252}, B. D. Pecjak

^{253}, M. Pelliccioni

^{254}, G. Perez

^{255}, L. Perrozzi

^{256}, F. Petriello

^{257}, G. Petrucciani

^{258}, E. Pianori

^{259}, F. Piccinini

^{260}, M. Pierini

^{261}, A. Pilkington

^{262}, S. Plätzer

^{263}, T. Plehn

^{264}, R. Podskubka

^{265}, C. T. Potter

^{266}, S. Pozzorini

^{267}, K. Prokofiev

^{268}, A. Pukhov

^{269}, I. Puljak

^{270}, M. Queitsch-Maitland

^{271}, J. Quevillon

^{272}, D. Rathlev

^{273}, M. Rauch

^{274}, E. Re

^{275}, M. N. Rebelo

^{276}, D. Rebuzzi

^{277}, L. Reina

^{278}, C. Reuschle

^{279}, J. Reuter

^{280}, M. Riembau

^{281}, F. Riva

^{282}, A. Rizzi

^{283}, T. Robens

^{284}, R. Röntsch

^{285}, J. Rojo

^{286}, J. C. Romão

^{287}, N. Rompotis

^{288}, J. Roskes

^{289}, R. Roth

^{290}, G. P. Salam

^{291}, R. Salerno

^{292}, R. Santos

^{293}, V. Sanz

^{294}, J. J. Sanz-Cillero

^{295}, H. Sargsyan

^{296}, U. Sarica

^{297}, P. Schichtel

^{298}, J. Schlenk

^{299}, T. Schmidt

^{300}, C. Schmitt

^{301}, M. Schönherr

^{302}, U. Schubert

^{303}, M. Schulze

^{304}, S. Sekula

^{305}, M. Sekulla

^{306}, E. Shabalina

^{307}, H. S. Shao

^{308}, J. Shelton

^{309}, C. H. Shepherd-Themistocleous

^{310}, S. Y. Shim

^{311}, F. Siegert

^{312}, A. Signer

^{313}, J. P. Silva

^{314}, L. Silvestrini

^{315}, M. Sjodahl

^{316}, P. Slavich

^{317}, M. Slawinska

^{318}, L. Soffi

^{319}, M. Spannowsky

^{320}, C. Speckner

^{321}, D. M. Sperka

^{322}, M. Spira

^{323}, O. Stål

^{324}, F. Staub

^{325}, T. Stebel

^{326}, T. Stefaniak

^{327}, M. Steinhauser

^{328}, I. W. Stewart

^{329}, M. J. Strassler

^{330}, J. Streicher

^{331}, D. M. Strom

^{332}, S. Su

^{333}, X. Sun

^{334}, F. J. Tackmann

^{335}, K. Tackmann

^{336}, A. M. Teixeira

^{337}, R. Teixeira de Lima

^{338}, V. Theeuwes

^{339}, R. Thorne

^{340}, D. Tommasini

^{341}, P. Torrielli

^{342}, M. Tosi

^{343}, F. Tramontano

^{344}, Z. Trócsányi

^{345}, M. Trott

^{346}, I. Tsinikos

^{347}, M. Ubiali

^{348}, P. Vanlaer

^{349}, W. Verkerke

^{350}, A. Vicini

^{351}, L. Viliani

^{352}, E. Vryonidou

^{353}, D. Wackeroth

^{354}, C. E. M. Wagner

^{355}, J. Wang

^{356}, S. Wayand

^{357}, G. Weiglein

^{358}, C. Weiss

^{359}, M. Wiesemann

^{360}, C. Williams

^{361}, J. Winter

^{362}, D. Winterbottom

^{363}, R. Wolf

^{364}, M. Xiao

^{365}, L. L. Yang

^{366}, R. Yohay

^{367}, S. P. Y. Yuen

^{368}, G. Zanderighi

^{369}, M. Zaro

^{370}, D. Zeppenfeld

^{371}, R. Ziegler

^{372}, T. Zirke

^{373}, J. Zupan

^{374}

**Affiliations:**

^{1}eds.,

^{2}eds.,

^{3}eds.,

^{4}eds.,

^{5}eds.,

^{6}eds.,

^{7}eds.,

^{8}eds.,

^{9}eds.,

^{10}The LHC Higgs Cross Section Working Group,

^{11}The LHC Higgs Cross Section Working Group,

^{12}The LHC Higgs Cross Section Working Group,

^{13}The LHC Higgs Cross Section Working Group,

^{14}The LHC Higgs Cross Section Working Group,

^{15}The LHC Higgs Cross Section Working Group,

^{16}The LHC Higgs Cross Section Working Group,

^{17}The LHC Higgs Cross Section Working Group,

^{18}The LHC Higgs Cross Section Working Group,

^{19}The LHC Higgs Cross Section Working Group,

^{20}The LHC Higgs Cross Section Working Group,

^{21}The LHC Higgs Cross Section Working Group,

^{22}The LHC Higgs Cross Section Working Group,

^{23}The LHC Higgs Cross Section Working Group,

^{24}The LHC Higgs Cross Section Working Group,

^{25}The LHC Higgs Cross Section Working Group,

^{26}The LHC Higgs Cross Section Working Group,

^{27}The LHC Higgs Cross Section Working Group,

^{28}The LHC Higgs Cross Section Working Group,

^{29}The LHC Higgs Cross Section Working Group,

^{30}The LHC Higgs Cross Section Working Group,

^{31}The LHC Higgs Cross Section Working Group,

^{32}The LHC Higgs Cross Section Working Group,

^{33}The LHC Higgs Cross Section Working Group,

^{34}The LHC Higgs Cross Section Working Group,

^{35}The LHC Higgs Cross Section Working Group,

^{36}The LHC Higgs Cross Section Working Group,

^{37}The LHC Higgs Cross Section Working Group,

^{38}The LHC Higgs Cross Section Working Group,

^{39}The LHC Higgs Cross Section Working Group,

^{40}The LHC Higgs Cross Section Working Group,

^{41}The LHC Higgs Cross Section Working Group,

^{42}The LHC Higgs Cross Section Working Group,

^{43}The LHC Higgs Cross Section Working Group,

^{44}The LHC Higgs Cross Section Working Group,

^{45}The LHC Higgs Cross Section Working Group,

^{46}The LHC Higgs Cross Section Working Group,

^{47}The LHC Higgs Cross Section Working Group,

^{48}The LHC Higgs Cross Section Working Group,

^{49}The LHC Higgs Cross Section Working Group,

^{50}The LHC Higgs Cross Section Working Group,

^{51}The LHC Higgs Cross Section Working Group,

^{52}The LHC Higgs Cross Section Working Group,

^{53}The LHC Higgs Cross Section Working Group,

^{54}The LHC Higgs Cross Section Working Group,

^{55}The LHC Higgs Cross Section Working Group,

^{56}The LHC Higgs Cross Section Working Group,

^{57}The LHC Higgs Cross Section Working Group,

^{58}The LHC Higgs Cross Section Working Group,

^{59}The LHC Higgs Cross Section Working Group,

^{60}The LHC Higgs Cross Section Working Group,

^{61}The LHC Higgs Cross Section Working Group,

^{62}The LHC Higgs Cross Section Working Group,

^{63}The LHC Higgs Cross Section Working Group,

^{64}The LHC Higgs Cross Section Working Group,

^{65}The LHC Higgs Cross Section Working Group,

^{66}The LHC Higgs Cross Section Working Group,

^{67}The LHC Higgs Cross Section Working Group,

^{68}The LHC Higgs Cross Section Working Group,

^{69}The LHC Higgs Cross Section Working Group,

^{70}The LHC Higgs Cross Section Working Group,

^{71}The LHC Higgs Cross Section Working Group,

^{72}The LHC Higgs Cross Section Working Group,

^{73}The LHC Higgs Cross Section Working Group,

^{74}The LHC Higgs Cross Section Working Group,

^{75}The LHC Higgs Cross Section Working Group,

^{76}The LHC Higgs Cross Section Working Group,

^{77}The LHC Higgs Cross Section Working Group,

^{78}The LHC Higgs Cross Section Working Group,

^{79}The LHC Higgs Cross Section Working Group,

^{80}The LHC Higgs Cross Section Working Group,

^{81}The LHC Higgs Cross Section Working Group,

^{82}The LHC Higgs Cross Section Working Group,

^{83}The LHC Higgs Cross Section Working Group,

^{84}The LHC Higgs Cross Section Working Group,

^{85}The LHC Higgs Cross Section Working Group,

^{86}The LHC Higgs Cross Section Working Group,

^{87}The LHC Higgs Cross Section Working Group,

^{88}The LHC Higgs Cross Section Working Group,

^{89}The LHC Higgs Cross Section Working Group,

^{90}The LHC Higgs Cross Section Working Group,

^{91}The LHC Higgs Cross Section Working Group,

^{92}The LHC Higgs Cross Section Working Group,

^{93}The LHC Higgs Cross Section Working Group,

^{94}The LHC Higgs Cross Section Working Group,

^{95}The LHC Higgs Cross Section Working Group,

^{96}The LHC Higgs Cross Section Working Group,

^{97}The LHC Higgs Cross Section Working Group,

^{98}The LHC Higgs Cross Section Working Group,

^{99}The LHC Higgs Cross Section Working Group,

^{100}The LHC Higgs Cross Section Working Group,

^{101}The LHC Higgs Cross Section Working Group,

^{102}The LHC Higgs Cross Section Working Group,

^{103}The LHC Higgs Cross Section Working Group,

^{104}The LHC Higgs Cross Section Working Group,

^{105}The LHC Higgs Cross Section Working Group,

^{106}The LHC Higgs Cross Section Working Group,

^{107}The LHC Higgs Cross Section Working Group,

^{108}The LHC Higgs Cross Section Working Group,

^{109}The LHC Higgs Cross Section Working Group,

^{110}The LHC Higgs Cross Section Working Group,

^{111}The LHC Higgs Cross Section Working Group,

^{112}The LHC Higgs Cross Section Working Group,

^{113}The LHC Higgs Cross Section Working Group,

^{114}The LHC Higgs Cross Section Working Group,

^{115}The LHC Higgs Cross Section Working Group,

^{116}The LHC Higgs Cross Section Working Group,

^{117}The LHC Higgs Cross Section Working Group,

^{118}The LHC Higgs Cross Section Working Group,

^{119}The LHC Higgs Cross Section Working Group,

^{120}The LHC Higgs Cross Section Working Group,

^{121}The LHC Higgs Cross Section Working Group,

^{122}The LHC Higgs Cross Section Working Group,

^{123}The LHC Higgs Cross Section Working Group,

^{124}The LHC Higgs Cross Section Working Group,

^{125}The LHC Higgs Cross Section Working Group,

^{126}The LHC Higgs Cross Section Working Group,

^{127}The LHC Higgs Cross Section Working Group,

^{128}The LHC Higgs Cross Section Working Group,

^{129}The LHC Higgs Cross Section Working Group,

^{130}The LHC Higgs Cross Section Working Group,

^{131}The LHC Higgs Cross Section Working Group,

^{132}The LHC Higgs Cross Section Working Group,

^{133}The LHC Higgs Cross Section Working Group,

^{134}The LHC Higgs Cross Section Working Group,

^{135}The LHC Higgs Cross Section Working Group,

^{136}The LHC Higgs Cross Section Working Group,

^{137}The LHC Higgs Cross Section Working Group,

^{138}The LHC Higgs Cross Section Working Group,

^{139}The LHC Higgs Cross Section Working Group,

^{140}The LHC Higgs Cross Section Working Group,

^{141}The LHC Higgs Cross Section Working Group,

^{142}The LHC Higgs Cross Section Working Group,

^{143}The LHC Higgs Cross Section Working Group,

^{144}The LHC Higgs Cross Section Working Group,

^{145}The LHC Higgs Cross Section Working Group,

^{146}The LHC Higgs Cross Section Working Group,

^{147}The LHC Higgs Cross Section Working Group,

^{148}The LHC Higgs Cross Section Working Group,

^{149}The LHC Higgs Cross Section Working Group,

^{150}The LHC Higgs Cross Section Working Group,

^{151}The LHC Higgs Cross Section Working Group,

^{152}The LHC Higgs Cross Section Working Group,

^{153}The LHC Higgs Cross Section Working Group,

^{154}The LHC Higgs Cross Section Working Group,

^{155}The LHC Higgs Cross Section Working Group,

^{156}The LHC Higgs Cross Section Working Group,

^{157}The LHC Higgs Cross Section Working Group,

^{158}The LHC Higgs Cross Section Working Group,

^{159}The LHC Higgs Cross Section Working Group,

^{160}The LHC Higgs Cross Section Working Group,

^{161}The LHC Higgs Cross Section Working Group,

^{162}The LHC Higgs Cross Section Working Group,

^{163}The LHC Higgs Cross Section Working Group,

^{164}The LHC Higgs Cross Section Working Group,

^{165}The LHC Higgs Cross Section Working Group,

^{166}The LHC Higgs Cross Section Working Group,

^{167}The LHC Higgs Cross Section Working Group,

^{168}The LHC Higgs Cross Section Working Group,

^{169}The LHC Higgs Cross Section Working Group,

^{170}The LHC Higgs Cross Section Working Group,

^{171}The LHC Higgs Cross Section Working Group,

^{172}The LHC Higgs Cross Section Working Group,

^{173}The LHC Higgs Cross Section Working Group,

^{174}The LHC Higgs Cross Section Working Group,

^{175}The LHC Higgs Cross Section Working Group,

^{176}The LHC Higgs Cross Section Working Group,

^{177}The LHC Higgs Cross Section Working Group,

^{178}The LHC Higgs Cross Section Working Group,

^{179}The LHC Higgs Cross Section Working Group,

^{180}The LHC Higgs Cross Section Working Group,

^{181}The LHC Higgs Cross Section Working Group,

^{182}The LHC Higgs Cross Section Working Group,

^{183}The LHC Higgs Cross Section Working Group,

^{184}The LHC Higgs Cross Section Working Group,

^{185}The LHC Higgs Cross Section Working Group,

^{186}The LHC Higgs Cross Section Working Group,

^{187}The LHC Higgs Cross Section Working Group,

^{188}The LHC Higgs Cross Section Working Group,

^{189}The LHC Higgs Cross Section Working Group,

^{190}The LHC Higgs Cross Section Working Group,

^{191}The LHC Higgs Cross Section Working Group,

^{192}The LHC Higgs Cross Section Working Group,

^{193}The LHC Higgs Cross Section Working Group,

^{194}The LHC Higgs Cross Section Working Group,

^{195}The LHC Higgs Cross Section Working Group,

^{196}The LHC Higgs Cross Section Working Group,

^{197}The LHC Higgs Cross Section Working Group,

^{198}The LHC Higgs Cross Section Working Group,

^{199}The LHC Higgs Cross Section Working Group,

^{200}The LHC Higgs Cross Section Working Group,

^{201}The LHC Higgs Cross Section Working Group,

^{202}The LHC Higgs Cross Section Working Group,

^{203}The LHC Higgs Cross Section Working Group,

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^{209}The LHC Higgs Cross Section Working Group,

^{210}The LHC Higgs Cross Section Working Group,

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^{212}The LHC Higgs Cross Section Working Group,

^{213}The LHC Higgs Cross Section Working Group,

^{214}The LHC Higgs Cross Section Working Group,

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^{216}The LHC Higgs Cross Section Working Group,

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^{220}The LHC Higgs Cross Section Working Group,

^{221}The LHC Higgs Cross Section Working Group,

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^{223}The LHC Higgs Cross Section Working Group,

^{224}The LHC Higgs Cross Section Working Group,

^{225}The LHC Higgs Cross Section Working Group,

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^{229}The LHC Higgs Cross Section Working Group,

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^{257}The LHC Higgs Cross Section Working Group,

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^{267}The LHC Higgs Cross Section Working Group,

^{268}The LHC Higgs Cross Section Working Group,

^{269}The LHC Higgs Cross Section Working Group,

^{270}The LHC Higgs Cross Section Working Group,

^{271}The LHC Higgs Cross Section Working Group,

^{272}The LHC Higgs Cross Section Working Group,

^{273}The LHC Higgs Cross Section Working Group,

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^{275}The LHC Higgs Cross Section Working Group,

^{276}The LHC Higgs Cross Section Working Group,

^{277}The LHC Higgs Cross Section Working Group,

^{278}The LHC Higgs Cross Section Working Group,

^{279}The LHC Higgs Cross Section Working Group,

^{280}The LHC Higgs Cross Section Working Group,

^{281}The LHC Higgs Cross Section Working Group,

^{282}The LHC Higgs Cross Section Working Group,

^{283}The LHC Higgs Cross Section Working Group,

^{284}The LHC Higgs Cross Section Working Group,

^{285}The LHC Higgs Cross Section Working Group,

^{286}The LHC Higgs Cross Section Working Group,

^{287}The LHC Higgs Cross Section Working Group,

^{288}The LHC Higgs Cross Section Working Group,

^{289}The LHC Higgs Cross Section Working Group,

^{290}The LHC Higgs Cross Section Working Group,

^{291}The LHC Higgs Cross Section Working Group,

^{292}The LHC Higgs Cross Section Working Group,

^{293}The LHC Higgs Cross Section Working Group,

^{294}The LHC Higgs Cross Section Working Group,

^{295}The LHC Higgs Cross Section Working Group,

^{296}The LHC Higgs Cross Section Working Group,

^{297}The LHC Higgs Cross Section Working Group,

^{298}The LHC Higgs Cross Section Working Group,

^{299}The LHC Higgs Cross Section Working Group,

^{300}The LHC Higgs Cross Section Working Group,

^{301}The LHC Higgs Cross Section Working Group,

^{302}The LHC Higgs Cross Section Working Group,

^{303}The LHC Higgs Cross Section Working Group,

^{304}The LHC Higgs Cross Section Working Group,

^{305}The LHC Higgs Cross Section Working Group,

^{306}The LHC Higgs Cross Section Working Group,

^{307}The LHC Higgs Cross Section Working Group,

^{308}The LHC Higgs Cross Section Working Group,

^{309}The LHC Higgs Cross Section Working Group,

^{310}The LHC Higgs Cross Section Working Group,

^{311}The LHC Higgs Cross Section Working Group,

^{312}The LHC Higgs Cross Section Working Group,

^{313}The LHC Higgs Cross Section Working Group,

^{314}The LHC Higgs Cross Section Working Group,

^{315}The LHC Higgs Cross Section Working Group,

^{316}The LHC Higgs Cross Section Working Group,

^{317}The LHC Higgs Cross Section Working Group,

^{318}The LHC Higgs Cross Section Working Group,

^{319}The LHC Higgs Cross Section Working Group,

^{320}The LHC Higgs Cross Section Working Group,

^{321}The LHC Higgs Cross Section Working Group,

^{322}The LHC Higgs Cross Section Working Group,

^{323}The LHC Higgs Cross Section Working Group,

^{324}The LHC Higgs Cross Section Working Group,

^{325}The LHC Higgs Cross Section Working Group,

^{326}The LHC Higgs Cross Section Working Group,

^{327}The LHC Higgs Cross Section Working Group,

^{328}The LHC Higgs Cross Section Working Group,

^{329}The LHC Higgs Cross Section Working Group,

^{330}The LHC Higgs Cross Section Working Group,

^{331}The LHC Higgs Cross Section Working Group,

^{332}The LHC Higgs Cross Section Working Group,

^{333}The LHC Higgs Cross Section Working Group,

^{334}The LHC Higgs Cross Section Working Group,

^{335}The LHC Higgs Cross Section Working Group,

^{336}The LHC Higgs Cross Section Working Group,

^{337}The LHC Higgs Cross Section Working Group,

^{338}The LHC Higgs Cross Section Working Group,

^{339}The LHC Higgs Cross Section Working Group,

^{340}The LHC Higgs Cross Section Working Group,

^{341}The LHC Higgs Cross Section Working Group,

^{342}The LHC Higgs Cross Section Working Group,

^{343}The LHC Higgs Cross Section Working Group,

^{344}The LHC Higgs Cross Section Working Group,

^{345}The LHC Higgs Cross Section Working Group,

^{346}The LHC Higgs Cross Section Working Group,

^{347}The LHC Higgs Cross Section Working Group,

^{348}The LHC Higgs Cross Section Working Group,

^{349}The LHC Higgs Cross Section Working Group,

^{350}The LHC Higgs Cross Section Working Group,

^{351}The LHC Higgs Cross Section Working Group,

^{352}The LHC Higgs Cross Section Working Group,

^{353}The LHC Higgs Cross Section Working Group,

^{354}The LHC Higgs Cross Section Working Group,

^{355}The LHC Higgs Cross Section Working Group,

^{356}The LHC Higgs Cross Section Working Group,

^{357}The LHC Higgs Cross Section Working Group,

^{358}The LHC Higgs Cross Section Working Group,

^{359}The LHC Higgs Cross Section Working Group,

^{360}The LHC Higgs Cross Section Working Group,

^{361}The LHC Higgs Cross Section Working Group,

^{362}The LHC Higgs Cross Section Working Group,

^{363}The LHC Higgs Cross Section Working Group,

^{364}The LHC Higgs Cross Section Working Group,

^{365}The LHC Higgs Cross Section Working Group,

^{366}The LHC Higgs Cross Section Working Group,

^{367}The LHC Higgs Cross Section Working Group,

^{368}The LHC Higgs Cross Section Working Group,

^{369}The LHC Higgs Cross Section Working Group,

^{370}The LHC Higgs Cross Section Working Group,

^{371}The LHC Higgs Cross Section Working Group,

^{372}The LHC Higgs Cross Section Working Group,

^{373}The LHC Higgs Cross Section Working Group,

^{374}The LHC Higgs Cross Section Working Group

This Report summarizes the results of the activities of the LHC Higgs Cross Section Working Group in the period 2014-2016. The main goal of the working group was to present the state-of-the-art of Higgs physics at the LHC, integrating all new results that have appeared in the last few years. The first part compiles the most up-to-date predictions of Higgs boson production cross sections and decay branching ratios, parton distribution functions, and off-shell Higgs boson production and interference effects. Read More

We analyze in detail a previous proposal by Dvali and G\'omez that black holes could be treated as consisting of a Bose-Einstein condensate of gravitons. In order to do so we extend the Einstein-Hilbert action with a chemical potential-like term, thus placing ourselves in a grand-canonical ensemble. The form and characteristics of this chemical potential-like piece are discussed in some detail. Read More

**Authors:**Antonio Dobado

^{1}, Rafael L. Delgado

^{2}, Felipe J. Llanes-Estrada

^{3}, Domenec Espriu

^{4}

**Affiliations:**

^{1}speaker, U. Complutense de Madrid,

^{2}speaker, U. Complutense de Madrid,

^{3}speaker, U. Complutense de Madrid,

^{4}U. Barcelona

**Category:**High Energy Physics - Phenomenology

Tantalizing LHC hints suggest that resonances of the Electroweak Symmetry Breaking Sector might exist at the TeV scale. We recall a few key meson-meson resonances in the GeV region that could have high-energy analogues which we compare, as well as the corresponding unitarized effective theories describing them. While detailed dynamics may be different, the constraints of unitarity, causality and global-symmetry breaking, incorporated in the Inverse Amplitude Method, allow to carry some intuition over to the largely unmeasured higher energy domain. Read More

A diboson excess has been observed ---albeit with very limited statistical significance--- in $WW$, $WZ$ and $ZZ$ final states at the LHC experiments using the accumulated 8 TeV data. Assuming that these signals are due to resonances resulting from an extended symmetry breaking sector in the standard model and exact custodial symmetry we determine using unitarization methods the values of the relevant low-energy constants in the corresponding effective Lagrangian. Unitarity arguments also predict the widths of these resonances. Read More

In this work we consider how the appearance of gradients of pseudoscalar condensates in dense systems may possibly influence the transport properties of photons in such a medium as well as other thermodynamic characteristics. We adopt the hypothesis that in regions where the pseudoscalar density gradient is large the properties of photons and fermions are governed by the usual lagrangian extended with a Chern-Simons interaction for photons and a constant axial field for fermions. We find that these new pieces in the lagrangian produce non-trivial reflection coefficients both for photons and fermions when entering or leaving a region where the pseudoscalar has a non-zero gradient. Read More

The scattering of longitudinally polarized W bosons in extensions of the Standard Model with anomalous Higgs couplings to the gauge sector and higher order $O(p^4)$ operators is considered. The modified couplings should be thought as the low energy remnants of some new dynamics involving the electroweak symmetry breaking sector. By imposing unitarity and causality constraints on $W_LW_L$ scattering amplitudes we relate the possible values of the effective couplings to the presence of new resonances above 300 GeV. Read More

Central heavy-ion collisions may induce sizeable fluctuations of the topological charge. This effect is expected to distort the dispersion relation for the hadron masses. We construct a general setup for a compact description of this phenomenon in the framework of bottom-up holographic approach to QCD. Read More

We study the Dine-Fischler-Srednicki (DFS) model in the light of the recent Higgs LHC results and electroweak precision data. The DFS model is a natural extension of the two-Higgs doublet model endowed with a Peccei-Quinn symmetry and leading to a physically acceptable axion. For generic couplings, the model reproduces the minimal Standard Model showing only tiny deviations (extreme decoupling scenario) whereas all additional degrees of freedom (with the exception of the axion) are very heavy. Read More

In this talk we will summarize the main results from our recent work concerning the possibility that a new metastable phase occurs in some heavy ion collisions (HIC). This phase would be characterized by the breaking of two characteristic symmetries of strong interactions; namely P and CP. We investigate the experimental consequences of parity breaking in such a situation and propose suitable observables to elucidate the presence this phenomenon. Read More

In this work we consider the effect that the appearance of pseudoscalar condensates in a neutron star can have on its cooling rate. We make no particular assumption on the origin and characteristics of these possible condensates and only assume that in regions where the pseudoscalar density varies the propagation of photons is governed by modified Maxwell-Chern-Simons electrodynamics. We find that this gives non-trivial reflection coefficients between regions of different pseudoscalar density and may affect very substantially the star cooling rate. Read More

We study the scattering of longitudinally polarized W bosons in extensions of the Standard Model where anomalous Higgs couplings to gauge sector and higher order O(p^4) operators are considered. These new couplings with respect to the Standard Model should be thought as the low energy remnants of some new dynamics involving the electroweak symmetry breaking sector. By imposing unitarity and causality constraints on the WW scattering amplitudes we find relevant restrictions on the possible values of the new couplings and the presence of new resonances above 300 GeV. Read More

We investigate how local parity breaking (LPB) due to large topological fluctuations may affect hadron physics. A distorted dispersion relation is derived for the lightest vector mesons $\rho$ and $\omega$. They are characterised by a mass splitting depending on their polarization. Read More

In this talk I review how a non-zero cosmological constant $\Lambda$ affects the propagation of gravitational waves and their detection in pulsar timing arrays (PTA). If $\Lambda\neq 0$ it turns out that waves are anharmonic in cosmological Friedmann-Robertson- Walker coordinates and although the amount of anharmonicity is very small it leads to potentially measurable effects. The timing residuals induced by gravitational waves in PTA would show a peculiar angular dependence with a marked enhancement around a particular value of the angle subtended by the source and the pulsars. Read More

In this work we analyze the propagation of photons in an environment where a strong magnetic field (perpendicular to the photon momenta) coexists with an oscillating cold axion background with the characteristics expected from dark matter in the galactic halo. Qualitatively, the main effect of the combined background is to produce a three-way mixing among the two photon polarizations and the axion. It is interesting to note that in spite of the extremely weak interaction of photons with the cold axion background, its effects compete with those coming from the magnetic field in some regions of the parameter space. Read More

**Authors:**R. Essig, J. A. Jaros, W. Wester, P. Hansson Adrian, S. Andreas, T. Averett, O. Baker, B. Batell, M. Battaglieri, J. Beacham, T. Beranek, J. D. Bjorken, F. Bossi, J. R. Boyce, G. D. Cates, A. Celentano, A. S. Chou, R. Cowan, F. Curciarello, H. Davoudiasl, P. deNiverville, R. De Vita, A. Denig, R. Dharmapalan, B. Dongwi, B. Döbrich, B. Echenard, D. Espriu, S. Fegan, P. Fisher, G. B. Franklin, A. Gasparian, Y. Gershtein, M. Graham, P. W. Graham, A. Haas, A. Hatzikoutelis, M. Holtrop, I. Irastorza, E. Izaguirre, J. Jaeckel, Y. Kahn, N. Kalantarians, M. Kohl, G. Krnjaic, V. Kubarovsky, H-S. Lee, A. Lindner, A. Lobanov, W. J. Marciano, D. J. E. Marsh, T. Maruyama, D. McKeen, H. Merkel, K. Moffeit, P. Monaghan, G. Mueller, T. K. Nelson, G. R. Neil, M. Oriunno, Z. Pavlovic, S. K. Phillips, M. J. Pivovaroff, R. Poltis, M. Pospelov, S. Rajendran, J. Redondo, A. Ringwald, A. Ritz, J. Ruz, K. Saenboonruang, P. Schuster, M. Shinn, T. R. Slatyer, J. H. Steffen, S. Stepanyan, D. B. Tanner, J. Thaler, M. E. Tobar, N. Toro, A. Upadye, R. Van de Water, B. Vlahovic, J. K. Vogel, D. Walker, A. Weltman, B. Wojtsekhowski, S. Zhang, K. Zioutas

Dark sectors, consisting of new, light, weakly-coupled particles that do not interact with the known strong, weak, or electromagnetic forces, are a particularly compelling possibility for new physics. Nature may contain numerous dark sectors, each with their own beautiful structure, distinct particles, and forces. This review summarizes the physics motivation for dark sectors and the exciting opportunities for experimental exploration. Read More

We consider the "two flavour" Nambu--Jona-Lasinio model in the presence of a vector and an axial external chemical potentials and study the phase structure of the model at zero temperature. The Nambu--Jona-Lasinio model is often used as a toy replica of QCD and it is therefore interesting to explore the consequences of adding external vector and axial chemical potentials in this model, mostly motivated by claims that such external drivers could trigger a phase where parity could be broken in QCD. We are also motivated by some lattice analysis that attempt to understand the nature of the so-called Aoki phase using this simplified model. Read More

Recent data on dilepton production in heavy ion collisions revealed an abnormal excess in the region of invariant masses below 1 GeV. Our proposal is the creation of a slowly varying time-dependent pseudoscalar condensate within the hot nuclear fireball that comes from the very collision. The local parity breaking effect that immediately arises substantially modifies the vector meson properties leading to an excess of lepton pairs that could be a part of the explanation for the observed abnormal dilepton yield. Read More

We consider the low energy realization of QCD in terms of meson fields when an axial chemical potential is present; a situation that may be relevant in heavy ion collisions. We shall demonstrate that the presence of an axial charge constitutes an explicit source of parity breaking. The eigenstates of strong interactions do not have a definite parity and interactions that would otherwise be forbidden compete with the familiar ones. Read More

We discuss some striking properties of photons propagating in a cold axion condensate oscillating coherently in time with a frequency $1/m_a$. Three effects are discussed in this contribution: (a) due to the time dependence of the background, photons moving in the cold axion background have no definite energies and some momenta are not accessible to them. (b) we investigate the combined influence of a magnetic field and the cold axion background and propose a possible interferometric experiment to detect the latter. Read More

The scattering of longitudinally polarized electroweak bosons is likely to play an important role in the elucidation of the fundamental nature of the Electroweak Symmetry Breaking sector and in determining the Higgs interactions with this sector. In this paper, by making use of the Equivalence Theorem, we determine the renormalization properties of the electroweak effective theory parameters in a model with generic Higgs couplings to the W and Z bosons. When the couplings between the Higgs and the electroweak gauge bosons deviate from their Standard Model values, additional counterterms of O(p^4) in the usual chiral counting are required. Read More

Our understanding of quantum gravity suggests that at the Planck scale the usual geometry loses its meaning. If so, the quest for grand unification in a large non-abelian group naturally endowed with the property of asymptotic freedom may also lose its motivation. Instead we propose an unification of all fundamental interactions at the Planck scale in the form of a Universal Landau Pole (ULP), at which all gauge couplings diverge. Read More

WW scattering is dominated at high energies by their longitudinal components, which are the most sensitive to the nature of the electroweak symmetry breaking. Prior to the discovery at the LHC of a Higgs-like particle, unitarization tools were extensively used to show that, in the absence of a light Higgs boson, new resonances resulting from the would-be strongly-interacting electroweak sector would appear, and furthermore these techniques would approximately predict their masses, widths, and signal strengths. With the discovery of a Higgs-like particle now firmly established, we re-investigate these techniques assuming this particle couples exactly as in the SM, but still being open to the possibility of an extended symmetry breaking sector. Read More

We investigate how large baryon densities (and possibly high temperatures) may induce spontaneous parity violation in the composite meson sector of vector-like gauge theory (presumably QCD or techni-QCD) . The analysis at intermediate energy scales is done by using an extended $\sigma$-model lagrangian that includes two scalar and two pseudoscalar multiplets and fulfills low-energy constraints for vector-like gauge theories. We elaborate on a novel mechanism of parity breaking based on the interplay between lightest and heavier meson condensates, which therefore cannot be realized in the simplest $\sigma$ model. Read More

We consider the low energy realization of QCD in terms of mesons when an axial chemical potential is present; a situation that may be relevant in heavy ion collisions. We shall demonstrate that the presence of an axial charge has profound consequences on meson physics. The most notorious effect is the appearance of an explicit source of parity breaking. Read More

We have considered the propagation of gravitational waves (GW) in de Sitter space time and how a non-zero value of the cosmological constant might affect their detection in pulsar timing arrays (PTA). If {\Lambda} is different from zero waves are non-linear in Friedmann-Robertson-Walker coordinates and although the amount of non-linearity is very small it gives noticeable effects for GW originating in extragalactic sources such as spiraling black hole binaries. The results indicate that the timing residuals induced by gravitational waves from such sources in PTA would show a peculiar angular dependence with a marked enhancement around a particular value of the angle subtended by the source and the pulsars, depending mainly on the actual value of the cosmological constant and the distance to the source. Read More

We present the extension to 4 dimensions of an euclidean 2-dimensional model that exhibits spontaneous generation of a metric. In this model gravitons emerge as Goldstone bosons of a global SO(D) X GL(D) symmetry broken down to SO(D). The microscopic theory can be formulated without having to appeal to any particular space-time metric and only assumes the pre-existence of a manifold endowed with an affine connection. Read More

We propose that local parity breaking induced by a large-scale fluctuation of topological charge at large temperatures and/or condensation of pseudoscalar mesons in the isotriplet channel for large baryon densities may be responsible for the substantial dilepton excess that is found for low invariant masses and moderate values of $p_T$ in central heavy ions collisions. This insofar unexplained enhancement could be understood by a combination of two effects leading both to an excess of $e^+e^-$ and $\mu^+ \mu^-$ pairs with respect to theoretical predictions based on conventional hadronic processes: (a) a modification of the dispersion relation of photons and vector mesons propagating in such a nuclear medium due to local parity breaking; (b) the appearance of new decay channels, forbidden by parity conservation in QCD in the usual vacuum. Possible signatures of this effect and perspectives for its detection are discussed. Read More

A cold relic axion condensate resulting from vacuum misalignment in the early universe oscillates with a frequency \sim m_a, where m_a is the axion mass. We summarize how the properties of photons propagating in such a medium are modified. Although the effects are small due to the magnitude of the axion-photon coupling, some consequences are striking. Read More

We derive the effects of a non-zero cosmological constant $\Lambda$ on gravitational wave propagation in the linearized approximation of general relativity. In this approximation we consider the situation where the metric can be written as $g_{\mu\nu}= \eta_{\mu\nu}+ h_{\mu\nu}^\Lambda + h_{\mu\nu}^W$, $h_{\mu\nu}^{\Lambda,W}<< 1$, where $h_{\mu\nu}^{\Lambda}$ is the background perturbation and $h_{\mu\nu}^{W}$ is a modification interpretable as a gravitational wave. For $\Lambda \neq 0$ this linearization of Einstein equations is self-consistent only in certain coordinate systems. Read More

A cold relic axion condensate resulting from vacuum misalignment in the early universe oscillates with a frequency m, where m is the axion mass. We determine the properties of photons propagating in a simplified version of such a background where the sinusoidal variation is replaced by a square wave profile. We prove that previous results that indicated that charged particles moving fast in such a background radiate, originally derived assuming that all momenta involved were much larger than m, hold for long wavelengths too. Read More

At finite density parity can be spontaneously broken in strong interactions with far reaching implications. In particular, a time-dependent pseudoscalar background would modify QED by adding a Chern-Simons term to the lagrangian. As a striking consequence we propose a novel explanation for the dilepton excess observed in heavy ion collisions at low invariant masses. Read More

We propose a novel explanation for the dilepton excess observed in heavy ion collisions at invariant masses below 1 GeV. We argue that the presence of local parity breaking due to a time-dependent isosinglet and/or isotriplet pseudoscalar condensate substantially modifies the dispersion relation of photons and vector mesons propagating in such a medium, changing the \rho~ spectral function and resulting in a potentially large excess of e+e- and \mu+\mu- with respect to the theoretical predictions based in a 'cocktail' of known hadronic processes. Possible signatures to prove or disprove this effect are discussed. Read More

We investigate the propagation of a charged particle in a spatially constant but time dependent pseudoscalar background. Physically this pseudoscalar background could be provided by a relic axion density. The background leads to an explicit breaking of Lorentz invariance; as a consequence processes such as $p\to p \gamma$ or $e\to e \gamma$ are possible within some kinematical constraints. Read More

In a previous work we investigated the propagation of fast moving charged particles in a spatially constant but slowly time dependent pseudoscalar background, such as the one provided by cold relic axions. The background induces cosmic rays to radiate in the low-energy spectrum. While the energy loss caused by this mechanism on the primary cosmic rays is negligible, we investigate the hypothetical detection of the photons radiated and how they could provide an indirect way of verifying the cosmological relevance of axions. Read More

We review the similarities between the effective chiral lagrangrian, relevant for low-energy strong interactions, and the Einstein-Hilbert action. We use these analogies to suggest a specific mechanism whereby gravitons would emerge as Goldstone bosons of a global SO(D) X GL(D) symmetry broken down to SO(D) by fermion condensation. We propose a two-dimensional toy model where a dynamical zwei-bein is generated from a topological theory without any pre-existing metric structure, the space being endowed only with an affine connection. Read More

We investigate the propagation of a charged particle in a spatially constant, but time dependent, pseudoscalar background. Physically this pseudoscalar background could be provided by a relic axion density. The background leads to an explicit breaking of Lorentz invariance; as a consequence the process p-> p gamma is possible and the background acts as a shield against extremely energetic cosmic rays, an effect somewhat similar to the GZK cut-off effect. Read More

**Category:**High Energy Physics - Theory

Using as inspiration the well known chiral effective lagrangian describing the interactions of pions at low energies, in these lectures we review the quantization procedure of Einstein gravity in the spirit of effective field theories. As has been emphasized by several authors, quantum corrections to observables in gravity are, by naive power counting, very small. While some quantities are not predictable (they require local counterterms of higher dimensionality) others, non local, are. Read More

We entertain the idea that a suitable background of cold (very low momentum) pseudoscalar particles or condensate, may trigger a background that effectively generates Lorentz-invariance violation. This aether-like background induces a Chern-Simons modification of QED. Physics is different in different frames and, in the rest frame of the pseudoscalar background, high momentum photons can decay into pairs. Read More

We investigate the possibility of parity being spontaneously violated in QCD at finite baryon density and temperature. The analysis is done for an idealized homogeneous and infinite nuclear matter where the influence of density can be examined with the help of constant chemical potential. QCD is approximated by a generalized sigma-model with two isomultiplets of scalars and pseudoscalars. Read More

We investigate the relation among slopes and intercepts of Regge trajectories for mesons of a given spin and different parities using large N_c arguments and the matching to perturbative QCD in the deep-Minkowski region. For spin-1 mesons of opposite parities we prove that: a) for large and increasing N_c, the scale \Lambda^{(V,A)} separating the resonance-dominated and the perturbative-saturated region in the channels V,A grows as \sqrt{N_c}; b) to satisfy the Weinberg sum rules the slopes of Regge trajectories for mesons of opposite parities must coincide; c) their intercepts may differ and their difference corresponds to the difference between \Lambda^V and \Lambda^A. Some arguments indicate that this difference should tend to zero as N_c\to\infty. Read More

**Affiliations:**

^{1}Universitat de Barcelona,

^{2}Universitat de Barcelona

**Category:**General Relativity and Quantum Cosmology

In this paper we revisit and extend a previous analysis where the possible relevance of quantum gravity effects in a cosmological setup was studied. The object of interest are non-local (logarithmic) terms generated in the effective action of gravity due to the exchange in loops of massless modes (such as photons or the gravitons themselves). We correct one mistake existing in the previous work and discuss the issue in a more general setting in different cosmological scenarios. Read More

We investigate possibilities for dynamical P-parity violation in dense baryon matter in the framework of effective quark models. Dynamical P-parity violation can appear in models with at least two scalar and two pseudoscalar fields, where both scalar fields are condensed at normal conditions. At special configurations of coupling constants, one of pseudoscalar fields can then also condense at some value of baryon density, the phenomenon results in mixing of the scalar and pseudoscalar physical degrees of freedom, hence, giving rise to P-parity violation. Read More

We show how the introduction of a finite baryon density may trigger spontaneous parity violation in the hadronic phase of QCD. Since this involves strong interaction physics in an intermediate energy range we approximate QCD by a \sigma model that retains the two lowest scalar and pseudoscalar multiplets. We propose a novel mechanism based on interplay between lightest and heavy meson states which cannot be realized solely in the Goldstone boson (pion) sector and thereby is unrelated to the one advocated by Migdal some time ago. Read More

We show how such important features of QCD as chiral symmetry breaking or the formation of a mass-gap can be directly traced from QCD sum rules for two point functions assuming, in the large number of colors limit, exact duality between the operator product expansion and the spectrum described by linearly (or nearly linear) rising Regge trajectories as predicted by string theory. We see how the presence of chiral symmetry breaking is intimately related to confinement in this scenario, as expected from general arguments, and how Regge trajectories change when chiral symmetry is broken. As a result the whole meson mass spectrum can be parametrized with a good accuracy by the constant $f_{\pi}$ only, thus realizing the program proposed by Migdal some time ago. Read More

We derive the the effective lagrangian that describes the interactions among vector, axial-vector mesons and pseudoscalars starting from the extended chiral quark model (ECQM). The results for the low-energy constants of this effective lagrangian have a parametric resemblance with existing predictions based on the Nambu-Jona-Lasinio model (except for some overall signs that we correct), but are numerically different. Therefore a precise measurement of these decay constants can shed some light on the way chiral symmetry breaking is modelled in QCD. Read More

We present an analysis of the gonihedric loop model, a reformulation of the two dimensional gonihedric spin model, using two different techniques. First, the usual regular lattice statistical physics problem is mapped onto a height model and studied analytically. Second, the gravitational version of this loop model is studied via matrix models techniques. Read More

We investigate the possible corrections to the linear Regge trajectories for the light-quark meson sector by matching two-point correlators of quark currents to the Operator Product Expansion. We find that the allowed modifications to the linear behavior must decrease rapidly with the principal quantum number. After fitting the lightest states in each channel and certain low-energy constants the whole spectrum for meson masses and residues is obtained in a satisfactory agreement with phenomenology. Read More

QCD at long distances can be described by the chiral Lagrangian. On the other hand there is overwhelming evidence that QCD and all non-abelian theories admit an effective string description. Here we review a derivation of the (intrinsic) parity-even chiral Lagrangian by requiring that the propagation of the QCD string takes place on a background where chiral symmetry is spontaneously broken. Read More

We study the one-loop effective action for gravity in a cosmological setup to determine possible cosmological effects of quantum corrections to Einstein theory. By considering the effect of the universal non-local terms in a toy model, we show that they can play an important role in the very early universe. We find that during inflation, the non-local terms are significant, leading to deviations from the standard inflationary expansion. Read More

**Affiliations:**

^{1}St.Petersburg State University & INFN, Bologna,

^{2}Departament d'ECM, Universitat de Barcelona,

^{3}Departament d'ECM, Universitat de Barcelona

The QCD hadronic string is supplemented with the reparameterization-invariant boundary interaction to background chiral fields associated with pions in a way compatible with the conformal symmetry. It allows the full reconstruction of the P-even part of the Chiral Lagrangian in a good agreement with the phenomenology of P-even meson interactions. The modification of boundary interaction necessary to induce the parity-odd Chiral Dynamics (WZW action) is outlined. Read More