SNO+ is a large liquid scintillator-based experiment located 2 km underground at SNOLAB, Sudbury, Canada. It reuses the Sudbury Neutrino Observatory detector, consisting of a 12 m diameter acrylic vessel which will be filled with about 780 tonnes of ultra-pure liquid scintillator. Designed as a multipurpose neutrino experiment, the primary goal of SNO+ is a search for the neutrinoless double-beta decay (0<svg xmlns:xlink="http://www.w3.org/1999/xlink" xmlns="http://www.w3.org/2000/svg" style="vertical-align:-3.42947pt" id="M1" height="12.7178pt" version="1.1" viewBox="-0.0498162 -9.28833 21.1864 12.7178" width="21.1864pt"><g transform="matrix(.013,0,0,-0.013,0,0)"><path id="g185-47" d="M213 67C239 136 257 225 255 300C253 353 242 447 164 447C112 447 54 389 41 319L67 309C90 362 117 377 134 377C184 377 189 277 190 239C193 153 164 43 146 -12H176C278 73 450 253 450 390C450 439 410 463 396 463C384 463 380 459 382 449C385 440 389 415 389 402C389 284 312 146 216 67H213Z"/></g><g transform="matrix(.013,0,0,-0.013,5.902,0)"><path id="g113-224" d="M558 587C558 666 497 712 432 712C379 712 330 691 284 650C212 586 178 508 148 348L71 -65C49 -185 35 -229 23 -235L27 -261C49 -259 101 -251 124 -224C131 -216 138 -178 159 -24C171 66 197 200 227 356C264 550 295 668 393 668C443 668 479 632 479 575C479 516 446 458 383 418C361 404 344 398 318 397L296 350C395 338 460 281 460 192C460 110 411 40 300 40C258 40 215 55 192 69L181 51C191 18 222 -16 266 -16C308 -16 351 1 397 26C471 67 545 142 545 221C545 315 486 365 401 395C469 437 558 498 558 587Z"/></g><g transform="matrix(.013,0,0,-0.013,13.456,0)"><use xlink:href="#g113-224"/></g></svg>) of <sup>130</sup>Te. In Phase I, the detector will be loaded with 0.3% natural tellurium, corresponding to nearly 800 kg of <sup>130</sup>Te, with an expected effective Majorana neutrino mass sensitivity in the region of 55–133 meV, just above the inverted mass hierarchy. Recently, the possibility of deploying up to ten times more natural tellurium has been investigated, which would enable SNO+ to achieve sensitivity deep into the parameter space for the inverted neutrino mass hierarchy in the future. Additionally, SNO+ aims to measure reactor antineutrino oscillations, low energy solar neutrinos, and geoneutrinos, to be sensitive to supernova neutrinos, and to search for exotic physics. A first phase with the detector filled with water will begin soon, with the scintillator phase expected to start after a few months of water data taking. The <svg xmlns:xlink="http://www.w3.org/1999/xlink" xmlns="http://www.w3.org/2000/svg" style="vertical-align:-3.42947pt" id="M2" height="12.7178pt" version="1.1" viewBox="-0.0498162 -9.28833 27.4498 12.7178" width="27.4498pt"><g transform="matrix(.013,0,0,-0.013,0,0)"><path id="g113-49" d="M241 635C89 635 35 457 35 312C35 153 89 -12 240 -12C390 -12 443 166 443 312C443 466 390 635 241 635ZM238 602C329 602 354 454 354 312C354 172 330 22 240 22C152 22 124 173 124 313S148 602 238 602Z"/></g><g transform="matrix(.013,0,0,-0.013,6.24,0)"><use xlink:href="#g185-47"/></g><g transform="matrix(.013,0,0,-0.013,12.142,0)"><use xlink:href="#g113-224"/></g><g transform="matrix(.013,0,0,-0.013,19.696,0)"><use xlink:href="#g113-224"/></g></svg> Phase I is foreseen for 2017.

S. Andringa

E. Arushanova

S. Asahi

M. Askins

D. J. Auty

A. R. Back

Z. Barnard

N. Barros

E. W. Beier

A. Bialek

S. D. Biller

E. Blucher

R. Bonventre

D. Braid

E. Caden

E. Callaghan

J. Caravaca

J. Carvalho

L. Cavalli

D. Chauhan

M. Chen

O. Chkvorets

K. Clark

B. Cleveland

I. T. Coulter

D. Cressy

X. Dai

C. Darrach

B. Davis-Purcell

R. Deen

M. M. Depatie

F. Descamps

F. Di Lodovico

N. Duhaime

F. Duncan

J. Dunger

E. Falk

N. Fatemighomi

R. Ford

P. Gorel

C. Grant

S. Grullon

E. Guillian

A. L. Hallin

D. Hallman

S. Hans

J. Hartnell

P. Harvey

M. Hedayatipour

W. J. Heintzelman

R. L. Helmer

B. Hreljac

J. Hu

T. Iida

C. M. Jackson

N. A. Jelley

C. Jillings

C. Jones

P. G. Jones

K. Kamdin

T. Kaptanoglu

J. Kaspar

P. Keener

P. Khaghani

L. Kippenbrock

J. R. Klein

R. Knapik

J. N. Kofron

L. L. Kormos

S. Korte

C. Kraus

C. B. Krauss

K. Labe

I. Lam

C. Lan

B. J. Land

S. Langrock

A. LaTorre

I. Lawson

G. M. Lefeuvre

E. J. Leming

J. Lidgard

X. Liu

Y. Liu

V. Lozza

S. Maguire

A. Maio

K. Majumdar

S. Manecki

J. Maneira

E. Marzec

A. Mastbaum

N. McCauley

A. B. McDonald

J. E. McMillan

P. Mekarski

C. Miller

Y. Mohan

E. Mony

M. J. Mottram

Current Status and Future Prospects of the SNO+ Experiment

We solve approximately Dirac equation for Eckart plus Hulthen potentials with Coulomb-like and Yukawa-like tensor interaction in the presence of spin and pseudospin symmetry for <svg xmlns:xlink="http://www.w3.org/1999/xlink" xmlns="http://www.w3.org/2000/svg" style="vertical-align:-1.23727pt" id="M1" height="10.5256pt" version="1.1" viewBox="-0.0498162 -9.28833 27.8499 10.5256" width="27.8499pt"><g transform="matrix(.013,0,0,-0.013,0,0)"><path id="g113-108" d="M480 416C480 431 465 448 438 448C388 448 312 383 252 330C217 299 188 273 155 237H153L257 680C262 700 263 712 253 712C240 712 183 684 97 674L92 648L126 647C166 646 172 645 163 606L23 -6L29 -12C51 -5 77 2 107 8C115 62 130 128 142 180C153 193 179 220 204 241C231 170 259 106 288 54C317 0 336 -12 358 -12C381 -12 423 2 477 80L460 100C434 74 408 54 398 54C385 54 374 65 351 107C326 154 282 241 263 299C296 332 351 377 403 377C424 377 436 372 445 368C449 366 456 368 462 375C472 386 480 402 480 416Z"/></g><g transform="matrix(.013,0,0,-0.013,17.844,0)"><path id="g117-145" d="M-161 592L-215 609L-427 -83L-372 -100L-161 592Z"/></g><g transform="matrix(.013,0,0,-0.013,10.171,0)"><path id="g117-34" d="M535 323V373H52V323H535ZM535 138V188H52V138H535Z"/></g><g transform="matrix(.013,0,0,-0.013,21.463,0)"><path id="g113-49" d="M241 635C89 635 35 457 35 312C35 153 89 -12 240 -12C390 -12 443 166 443 312C443 466 390 635 241 635ZM238 602C329 602 354 454 354 312C354 172 330 22 240 22C152 22 124 173 124 313S148 602 238 602Z"/></g></svg>. The formula method is used to obtain the energy eigenvalues and wave functions. We also discuss the energy eigenvalues and the Dirac spinors for Eckart plus Hulthen potentials with formula method. To show the accuracy of the present model, some numerical results are shown in both pseudospin and spin symmetry limits.

Mohammad Reza Shojaei

Mohsen Mousavi

The Effect of Tensor Interaction in Splitting the Energy Levels of Relativistic Systems

The full energy shift of a massive Dirac neutrino in magnetized electron-positron plasma was investigated using the Matsubara imaginary time and real time formalisms. The neutrino dispersion in the magnetized medium was analyzed as a function of the neutrino spin and mass. It was shown that in a superstrong magnetic field the CP-symmetric plasma contribution to the neutrino energy greatly exceeds the analogous correction in the field-free case. The contribution of plasma to the anomalous magnetic moment of a neutrino was obtained.

P. A. Eminov

Neutrino Spin and Dispersion in Magnetized Medium

Using the noncanonical model of scalar field, the cosmological consequences of a pervasive, self-interacting, homogeneous, and rolling scalar field are studied. In this model, the scalar field potential is “nonlinear” and decreases in magnitude with increasing the value of the scalar field. A special solution of the nonlinear field equations of <svg xmlns:xlink="http://www.w3.org/1999/xlink" xmlns="http://www.w3.org/2000/svg" style="vertical-align:-3.42948pt" id="M1" height="12.3916pt" version="1.1" viewBox="-0.0498162 -8.96212 7.47216 12.3916" width="7.47216pt"><g transform="matrix(.013,0,0,-0.013,0,0)"><path id="g113-243" d="M542 242C542 369 469 429 379 468C370 472 372 496 376 513L416 681L400 691L344 648L219 51C167 69 113 128 113 217C113 324 166 387 266 428L252 459C124 418 23 336 23 202C23 95 90 13 205 -8L182 -132C165 -222 191 -254 209 -261L215 -258L270 -7C415 -4 542 98 542 242ZM469 232C469 126 403 33 279 39L355 409C399 394 469 331 469 232Z"/></g></svg> that has time dependency as fixed point is obtained. The fixed point relies on the noncanonical term of action and <svg xmlns:xlink="http://www.w3.org/1999/xlink" xmlns="http://www.w3.org/2000/svg" style="vertical-align:-3.42943pt" id="M2" height="9.39034pt" version="1.1" viewBox="-0.0498162 -5.96091 6.63704 9.39034" width="6.63704pt"><g transform="matrix(.013,0,0,-0.013,0,0)"><path id="g113-225" d="M478 372C478 418 458 448 431 448C409 448 389 431 389 410C389 404 391 400 394 395C398 388 406 371 406 348C406 253 308 122 251 51H249C254 122 249 257 231 336C212 421 189 448 159 448C126 448 75 412 23 327L48 306C83 354 103 371 115 371C125 371 134 360 144 334C185 224 192 64 183 -19C146 -100 116 -202 110 -244L125 -261C154 -259 208 -234 222 -220C222 -194 225 -84 235 -23C247 -3 273 36 308 79C379 165 478 288 478 372Z"/></g></svg>-parameter; this parameter appeared in energy density of scalar field redshift. By means of such fixed point the different eigenvalues of the equation of motion will be obtained. In different epochs in the evolution of the Universe for different values of <svg xmlns:xlink="http://www.w3.org/1999/xlink" xmlns="http://www.w3.org/2000/svg" style="vertical-align:-3.42943pt" id="M3" height="9.39034pt" version="1.1" viewBox="-0.0498162 -5.96091 6.50656 9.39034" width="6.50656pt"><g transform="matrix(.013,0,0,-0.013,0,0)"><path id="g113-114" d="M474 429L457 433C435 440 389 448 367 448C348 448 323 446 309 443C266 434 195 406 148 366C78 307 23 210 23 101C23 35 55 -12 92 -12C118 -12 146 1 196 35C247 70 311 130 346 173H348L281 -148C268 -211 256 -221 208 -229L191 -232L187 -257L433 -245L437 -219L411 -216C357 -210 350 -205 362 -140L427 207C447 315 461 381 474 429ZM387 387C379 337 363 262 355 236C318 180 201 57 142 57C126 57 112 81 112 128C112 205 150 321 220 376C244 395 280 403 312 403C345 403 370 396 387 387Z"/></g></svg> and <svg xmlns:xlink="http://www.w3.org/1999/xlink" xmlns="http://www.w3.org/2000/svg" style="vertical-align:-0.2063904pt" id="M4" height="6.1673pt" version="1.1" viewBox="-0.0498162 -5.96091 6.6501 6.1673" width="6.6501pt"><g transform="matrix(.013,0,0,-0.013,0,0)"><path id="g113-111" d="M495 86L479 114C446 82 419 66 409 66C401 66 401 72 406 97C420 166 436 231 453 297C489 435 454 448 428 448C406 448 384 439 354 422C305 394 222 327 161 247H159L183 345C200 415 194 448 173 448C143 448 82 410 23 351L38 325C64 349 95 371 105 371C111 371 116 365 109 336L25 -4L31 -12C50 -4 77 3 107 9C119 69 132 122 145 168C197 254 321 381 370 381C387 381 393 374 378 305L329 95C309 17 320 -12 345 -12C372 -12 430 19 495 86Z"/></g></svg>, the potentials as a function of scalar field are attained. The behavior of baryonic perturbations in linear perturbation scenario as a considerable amount of energy density of scalar field at low redshifts prevents the growth of perturbations in the ordinary matter fluid. The energy density in the scalar field is not appreciably perturbed by nonrelativistic gravitational fields, in either the radiation or matter dominant or scalar field dominated epoch. 

Z. Ossoulian

T. Golanbari

H. Sheikhahmadi

Kh. Saaidi

Stability of a Noncanonical Scalar Field Model during Cosmological Date

The constraints imposed on the Minimal Supersymmetric Standard Model (MSSM) parameter space by the Large Hadron Collider (LHC) Higgs mass limit and gluino mass lower bound are revisited. We also analyze the thermal relic abundance of lightest neutralino, which is the Lightest Supersymmetric Particle (LSP). We show that the combined LHC and relic abundance constraints rule out most of the MSSM parameter space except a very narrow region with very large <svg xmlns:xlink="http://www.w3.org/1999/xlink" xmlns="http://www.w3.org/2000/svg" style="vertical-align:-3.42947pt" id="M1" height="12.7178pt" version="1.1" viewBox="-0.0498162 -9.28833 26.6668 12.7178" width="26.6668pt"><g transform="matrix(.013,0,0,-0.013,0,0)"><path id="g121-114" d="M298 36L289 62C276 55 253 45 228 45C202 45 169 60 169 141V397H276C289 405 292 426 282 437H169V574L155 576L90 509V437H45L17 408L21 397H90V107C90 28 125 -12 188 -12C198 -12 213 -8 230 1L298 36Z"/></g><g transform="matrix(.013,0,0,-0.013,4.043,0)"><path id="g121-95" d="M433 39L423 65C413 59 399 54 387 54C370 54 352 69 352 114V299C352 352 342 392 307 422C285 440 255 449 225 449C168 437 102 399 75 379C56 365 44 353 44 339C44 315 69 296 87 296C101 296 111 303 116 319C124 349 133 371 145 385C156 397 171 404 190 404C241 404 275 364 275 291V274C253 256 180 229 120 209C65 190 39 159 39 110C39 47 88 -12 159 -12C189 -12 237 25 277 52C282 35 288 21 301 8C312 -3 333 -12 348 -12L433 39ZM275 84C256 65 221 48 195 48C164 48 124 73 124 124C124 161 146 180 185 198C206 208 254 229 275 240V84Z"/></g><g transform="matrix(.013,0,0,-0.013,9.633,0)"><path id="g121-108" d="M524 0V26C466 32 460 36 460 104V297C460 393 411 449 331 449C302 449 276 437 248 419C223 402 201 387 181 372V451C137 432 90 420 42 411V388C96 378 102 374 102 310V104C102 38 97 33 29 26V0H246V26C187 32 181 36 181 104V339C211 365 250 390 290 390C357 390 381 345 381 276V109C381 40 374 32 315 26V0H524Z"/></g><g transform="matrix(.013,0,0,-0.013,18.986,0)"><path id="g113-224" d="M558 587C558 666 497 712 432 712C379 712 330 691 284 650C212 586 178 508 148 348L71 -65C49 -185 35 -229 23 -235L27 -261C49 -259 101 -251 124 -224C131 -216 138 -178 159 -24C171 66 197 200 227 356C264 550 295 668 393 668C443 668 479 632 479 575C479 516 446 458 383 418C361 404 344 398 318 397L296 350C395 338 460 281 460 192C460 110 411 40 300 40C258 40 215 55 192 69L181 51C191 18 222 -16 266 -16C308 -16 351 1 397 26C471 67 545 142 545 221C545 315 486 365 401 395C469 437 558 498 558 587Z"/></g></svg>  (~50). Within this region, we emphasize that the spin-independent scattering cross section of the LSP with a proton is less than the latest Large Underground Xenon (LUX) limit by at least two orders of magnitude. Finally, we argue that nonthermal Dark Matter (DM) scenario may relax the constraints imposed on the MSSM parameter space. Namely, the following regions are obtained: <svg xmlns:xlink="http://www.w3.org/1999/xlink" xmlns="http://www.w3.org/2000/svg" style="vertical-align:-3.29107pt" id="M2" height="12.5794pt" version="1.1" viewBox="-0.0498162 -9.28833 54.5225 12.5794" width="54.5225pt"><g transform="matrix(.013,0,0,-0.013,0,0)"><path id="g113-110" d="M766 88L752 113C719 83 690 64 681 64C674 64 672 74 679 103L724 292C758 436 724 448 701 448C680 448 666 442 639 429C594 407 514 350 441 252H439L447 289C476 423 450 448 419 448C398 448 379 441 355 427C307 400 234 344 162 249H160L180 324C203 409 197 448 170 448C144 448 82 413 23 349L35 321C57 343 96 374 108 374C115 374 117 371 111 341C87 227 57 112 24 -6L32 -12C53 -4 81 4 108 6C119 68 134 128 149 171C177 229 309 383 364 383C387 383 388 355 373 282C354 190 330 92 303 -6L309 -12C332 -4 356 3 386 6C396 63 411 122 424 171C458 236 590 383 642 383C658 383 664 369 652 315L603 91C587 20 593 -12 619 -12C642 -12 708 23 766 88Z"/></g><g transform="matrix(.0091,0,0,-0.0091,10.192,3.132)"><path id="g50-49" d="M245 635C92 635 37 457 37 312C37 149 91 -12 244 -12C395 -12 449 166 449 312C449 469 395 635 245 635ZM243 598C332 598 358 454 358 312C358 173 334 26 245 26C158 26 128 174 128 313S152 598 243 598Z"/></g><g transform="matrix(.013,0,0,-0.013,18.77,0)"><path id="g117-134" d="M535 138V188H52V138H535ZM536 353L507 390C486 357 454 333 416 333C388 333 343 353 308 370C264 391 211 414 171 414C121 414 78 382 49 340L80 307C100 339 133 364 171 364C197 364 244 343 279 326C323 305 374 283 416 283C465 283 506 314 536 353Z"/></g><g transform="matrix(.013,0,0,-0.013,30.033,0)"><path id="g198-16" d="M663 549C663 621 608 680 521 680C283 680 82 444 82 188C82 80 142 -15 258 -15C466 -15 637 203 637 396C637 502 561 542 497 542C414 542 336 469 336 362C336 331 339 284 371 232L393 242C369 289 366 322 366 347C366 448 430 506 494 506C539 506 586 470 586 396C586 266 508 157 469 118C409 57 343 15 256 15C179 15 142 78 142 150C142 331 347 645 517 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transform="matrix(.0091,0,0,-0.0091,10.192,3.132)"><path id="g50-50" d="M389 0V32C297 38 291 46 291 118V635C234 613 175 595 109 583V556L161 554C203 552 207 547 207 497V118C207 46 201 38 110 32V0H389Z"/></g><g transform="matrix(.0091,0,0,-0.0091,14.624,3.132)"><path id="g50-48" d="M381 704H317L48 -163H112L381 704Z"/></g><g transform="matrix(.0091,0,0,-0.0091,18.531,3.132)"><path id="g50-51" d="M414 144C384 79 371 75 317 75H135L276 221C367 316 408 376 408 465C408 570 327 635 237 635C179 635 131 609 100 575L42 494L67 471C94 510 138 565 205 565C277 565 321 517 321 435C321 348 258 270 195 195C146 137 88 81 33 26V0H411C423 44 433 88 446 135L414 144Z"/></g><g transform="matrix(.013,0,0,-0.013,27.137,0)"><use xlink:href="#g117-134"/></g><g transform="matrix(.013,0,0,-0.013,38.4,0)"><path id="g113-55" d="M137 343C167 482 260 545 321 574C357 591 397 603 429 609L423 641C382 634 335 622 295 608C189 570 37 457 37 238C37 84 125 -12 242 -12C362 -12 447 89 447 209C447 311 374 393 267 393C247 393 226 386 204 376L137 343ZM227 337C318 337 361 256 361 173C361 105 336 22 258 22C176 22 126 120 126 240C126 266 127 291 132 310C155 323 189 337 227 337Z"/></g><g transform="matrix(.013,0,0,-0.013,44.64,0)"><path id="g113-49" d="M241 635C89 635 35 457 35 312C35 153 89 -12 240 -12C390 -12 443 166 443 312C443 466 390 635 241 635ZM238 602C329 602 354 454 354 312C354 172 330 22 240 22C152 22 124 173 124 313S148 602 238 602Z"/></g><g transform="matrix(.013,0,0,-0.013,50.88,0)"><use xlink:href="#g113-49"/></g></svg> GeV for low <svg xmlns:xlink="http://www.w3.org/1999/xlink" xmlns="http://www.w3.org/2000/svg" style="vertical-align:-3.42947pt" id="M4" height="12.7178pt" version="1.1" viewBox="-0.0498162 -9.28833 26.6668 12.7178" width="26.6668pt"><g transform="matrix(.013,0,0,-0.013,0,0)"><use xlink:href="#g121-114"/></g><g transform="matrix(.013,0,0,-0.013,4.043,0)"><use xlink:href="#g121-95"/></g><g transform="matrix(.013,0,0,-0.013,9.633,0)"><use xlink:href="#g121-108"/></g><g transform="matrix(.013,0,0,-0.013,18.986,0)"><use xlink:href="#g113-224"/></g></svg>  (~10); <svg xmlns:xlink="http://www.w3.org/1999/xlink" xmlns="http://www.w3.org/2000/svg" style="vertical-align:-4.67947pt" id="M5" height="13.9678pt" version="1.1" viewBox="-0.0498162 -9.28833 92.9893 13.9678" width="92.9893pt"><g transform="matrix(.013,0,0,-0.013,0,0)"><use xlink:href="#g113-110"/></g><g transform="matrix(.0091,0,0,-0.0091,10.192,3.132)"><use xlink:href="#g50-49"/></g><g transform="matrix(.013,0,0,-0.013,18.77,0)"><path id="g117-131" d="M548 311L516 323C497 274 452 240 400 240C372 240 342 260 316 278C277 305 235 330 188 330C116 330 66 268 40 199L72 187C91 236 136 270 188 270C216 270 246 250 272 232C311 205 353 180 400 180C472 180 522 242 548 311Z"/></g><g transform="matrix(.013,0,0,-0.013,30.033,0)"><use xlink:href="#g113-110"/></g><g transform="matrix(.0091,0,0,-0.0091,40.225,3.132)"><use xlink:href="#g50-50"/></g><g transform="matrix(.0091,0,0,-0.0091,44.657,3.132)"><use xlink:href="#g50-48"/></g><g transform="matrix(.0091,0,0,-0.0091,48.564,3.132)"><use xlink:href="#g50-51"/></g><g transform="matrix(.013,0,0,-0.013,57.17,0)"><use xlink:href="#g117-134"/></g><g transform="matrix(.013,0,0,-0.013,68.433,0)"><use xlink:href="#g198-16"/></g><g transform="matrix(.013,0,0,-0.013,77.429,0)"><use xlink:href="#g113-41"/></g><g transform="matrix(.013,0,0,-0.013,81.927,0)"><path id="g113-50" d="M384 0V27C293 34 287 42 287 114V635C232 613 172 594 109 583V559L157 557C201 555 205 550 205 499V114C205 42 199 34 109 27V0H384Z"/></g><g transform="matrix(.013,0,0,-0.013,88.167,0)"><use xlink:href="#g113-42"/></g></svg> TeV or <svg xmlns:xlink="http://www.w3.org/1999/xlink" xmlns="http://www.w3.org/2000/svg" style="vertical-align:-3.29107pt" id="M6" height="12.5794pt" version="1.1" viewBox="-0.0498162 -9.28833 54.5225 12.5794" width="54.5225pt"><g transform="matrix(.013,0,0,-0.013,0,0)"><use xlink:href="#g113-110"/></g><g transform="matrix(.0091,0,0,-0.0091,10.192,3.132)"><use xlink:href="#g50-49"/></g><g transform="matrix(.013,0,0,-0.013,18.77,0)"><use xlink:href="#g117-134"/></g><g transform="matrix(.013,0,0,-0.013,30.033,0)"><use xlink:href="#g198-16"/></g><g transform="matrix(.013,0,0,-0.013,39.029,0)"><use xlink:href="#g113-41"/></g><g transform="matrix(.013,0,0,-0.013,43.527,0)"><use xlink:href="#g113-53"/></g><g transform="matrix(.013,0,0,-0.013,49.767,0)"><use xlink:href="#g113-42"/></g></svg> TeV and <svg xmlns:xlink="http://www.w3.org/1999/xlink" xmlns="http://www.w3.org/2000/svg" style="vertical-align:-4.679481pt" id="M7" height="13.0283pt" version="1.1" viewBox="-0.0498162 -8.34882 57.3566 13.0283" width="57.3566pt"><g transform="matrix(.013,0,0,-0.013,0,0)"><use xlink:href="#g113-110"/></g><g transform="matrix(.0091,0,0,-0.0091,10.192,3.132)"><use xlink:href="#g50-50"/></g><g transform="matrix(.0091,0,0,-0.0091,14.624,3.132)"><use xlink:href="#g50-48"/></g><g transform="matrix(.0091,0,0,-0.0091,18.531,3.132)"><use xlink:href="#g50-51"/></g><g transform="matrix(.013,0,0,-0.013,27.137,0)"><use xlink:href="#g117-134"/></g><g transform="matrix(.013,0,0,-0.013,38.4,0)"><path id="g113-56" d="M447 623H65C61 580 56 530 47 475H76C100 541 106 550 172 550H388C308 376 196 170 91 -1L98 -12L172 -2C268 204 360 408 455 611L447 623Z"/></g><g transform="matrix(.013,0,0,-0.013,44.642,0)"><use xlink:href="#g113-49"/></g><g transform="matrix(.013,0,0,-0.013,50.882,0)"><use xlink:href="#g113-49"/></g></svg> GeV for large <svg xmlns:xlink="http://www.w3.org/1999/xlink" xmlns="http://www.w3.org/2000/svg" style="vertical-align:-3.42947pt" id="M8" height="12.7178pt" version="1.1" viewBox="-0.0498162 -9.28833 26.6668 12.7178" width="26.6668pt"><g transform="matrix(.013,0,0,-0.013,0,0)"><use xlink:href="#g121-114"/></g><g transform="matrix(.013,0,0,-0.013,4.043,0)"><use xlink:href="#g121-95"/></g><g transform="matrix(.013,0,0,-0.013,9.633,0)"><use xlink:href="#g121-108"/></g><g transform="matrix(.013,0,0,-0.013,18.986,0)"><use xlink:href="#g113-224"/></g></svg>  (~50).

W. Abdallah

S. Khalil

MSSM Dark Matter in Light of Higgs and LUX Results

The Hawking radiation spectrum of Kerr-Sen axion-dilaton black holes is derived, in the context of dark spinors tunnelling across the horizon. Since a black hole has a well defined temperature, it should radiate in principle all the standard model particles, similar to a black body at that temperature. We investigate the tunnelling of mass dimension one spin-1/2 dark fermions, which are beyond the standard model and are prime candidates to the dark matter. Their interactions with the standard model matter and gauge fields are suppressed by at least one power of unification scale, being restricted just to the Higgs field and to the graviton likewise. The tunnelling method for the emission and absorption of mass dimension one particles across the event horizon of Kerr-Sen axion-dilaton black holes is shown here to provide further evidence for the universality of black hole radiation, further encompassing particles beyond the standard model.

R. T. Cavalcanti

Rold&#xe3;o da Rocha

Dark Spinors Hawking Radiation in String Theory Black Holes

We study the transverse momentum spectra of <svg xmlns:xlink="http://www.w3.org/1999/xlink" xmlns="http://www.w3.org/2000/svg" style="vertical-align:-3.42947pt" id="M1" height="12.7178pt" version="1.1" viewBox="-0.0498162 -9.28833 19.9076 12.7178" width="19.9076pt"><g transform="matrix(.013,0,0,-0.013,0,0)"><path id="g113-75" d="M429 650H175L169 622C251 614 259 612 244 532L174 152C163 91 152 37 135 -6C109 -72 67 -101 23 -113L33 -144C45 -143 73 -134 102 -119C186 -76 229 -1 254 133L327 532C341 609 347 613 423 622L429 650Z"/></g><g transform="matrix(.013,0,0,-0.013,5.879,0)"><path id="g113-48" d="M368 703H309L44 -163H104L368 703Z"/></g><g transform="matrix(.013,0,0,-0.013,11.24,0)"><path id="g113-245" d="M642 419L635 448C586 435 552 411 532 392C518 379 509 351 496 304C484 260 462 196 445 150C424 93 388 40 314 30L413 508L406 510L344 491L257 36C205 46 175 84 175 169C175 195 180 241 185 277C189 304 190 331 190 358C190 413 175 448 141 448C111 448 69 429 23 373L30 347C51 365 68 375 81 375C93 375 108 368 108 327C108 307 104 268 101 239C98 211 95 180 95 155C95 33 159 -8 248 -14L213 -186C206 -220 221 -254 230 -261L261 -230L306 -11C339 -4 366 6 389 20C431 46 473 87 503 155C533 224 557 286 571 325C586 367 606 393 642 419Z"/></g></svg> and <svg xmlns:xlink="http://www.w3.org/1999/xlink" xmlns="http://www.w3.org/2000/svg" style="vertical-align:-0.0498209pt" id="M2" height="8.68572pt" version="1.1" viewBox="-0.0498162 -8.6359 8.64656 8.68572" width="8.64656pt"><g transform="matrix(.013,0,0,-0.013,0,0)"><path id="g113-149" d="M648 625C638 644 619 665 597 665C518 665 445 585 404 489C377 436 359 379 345 309H340C335 367 324 448 296 515C263 599 214 665 123 665C83 665 33 649 1 632L6 606C19 608 32 609 44 609C124 609 186 567 230 473C270 390 283 308 283 200V122C283 42 274 33 184 27V0H468V27C376 33 368 42 368 122V194C368 293 402 401 461 492C512 573 576 611 629 611C634 611 636 611 642 610L648 625Z"/></g></svg> mesons by using two methods: the two-component Erlang distribution and the two-component Schwinger mechanism. The results obtained by the two methods are compared and found to be in agreement with the experimental data of proton-proton (<svg xmlns:xlink="http://www.w3.org/1999/xlink" xmlns="http://www.w3.org/2000/svg" style="vertical-align:-3.42943pt" id="M3" height="10.2124pt" version="1.1" viewBox="-0.0498162 -6.78297 14.662 10.2124" width="14.662pt"><g transform="matrix(.013,0,0,-0.013,0,0)"><path id="g113-113" d="M570 304C570 398 525 448 414 448C385 448 343 445 312 434L329 511L321 518C297 504 262 482 244 460L233 411C195 397 159 381 128 358L135 332C160 347 189 360 224 373L111 -147C97 -210 84 -218 17 -231L13 -257L254 -247L259 -218L233 -216C183 -212 177 -202 189 -142L218 -1C238 -10 266 -12 283 -12C351 3 429 48 483 105C543 168 570 242 570 304ZM482 289C482 161 380 33 304 33C278 33 248 51 233 69L303 396C326 400 352 403 369 403C428 403 482 380 482 289Z"/></g><g transform="matrix(.013,0,0,-0.013,6.797,0)"><use xlink:href="#g113-113"/></g></svg>), proton-lead (<svg xmlns:xlink="http://www.w3.org/1999/xlink" xmlns="http://www.w3.org/2000/svg" style="vertical-align:-3.42943pt" id="M4" height="10.2124pt" version="1.1" viewBox="-0.0498162 -6.78297 7.83752 10.2124" width="7.83752pt"><g transform="matrix(.013,0,0,-0.013,0,0)"><use xlink:href="#g113-113"/></g></svg>-Pb), and lead-lead (Pb-Pb) collisions measured by the LHCb and ALICE Collaborations at the large hadron collider (LHC). The related parameters such as the mean transverse momentum contributed by each parton in the first (second) component in the two-component Erlang distribution and the string tension between two partons in the first (second) component in the two-component Schwinger mechanism are extracted.

Li-Na Gao

Fu-Hu Liu

Comparing Erlang Distribution and Schwinger Mechanism on Transverse Momentum Spectra in High Energy Collisions

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<p><em>Advances in High Energy Physics</em> publishes the results of theoretical and experimental research on the nature of, and interaction between, energy and matter.</p>


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<p>Chief Editor, Professor Seidel, is a professor in the Department of Physics and Astronomy at the University of New Mexico. She is a collaborator on the ATLAS experiment at the Large Hadron Collider, researching high-energy collider physics.</p>


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Advances in High Energy Physics publishes the results of theoretical and experimental research on the nature of, and interaction between, energy and matter.

Advances in High Energy Physics