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Baryogenesis in theories with large extra spatial dimensions

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Published

Standard

Baryogenesis in theories with large extra spatial dimensions. / Allahverdi, Rouzbeh; Enqvist, Kari; Mazumdar, Anupam et al.
In: Nuclear Physics B, Vol. 618, No. 1-2, 10.12.2001, p. 277-300.

Research output: Contribution to Journal/MagazineJournal articlepeer-review

Harvard

Allahverdi, R, Enqvist, K, Mazumdar, A & Pérez-Lorenzana, A 2001, 'Baryogenesis in theories with large extra spatial dimensions', Nuclear Physics B, vol. 618, no. 1-2, pp. 277-300. https://doi.org/10.1016/S0550-3213(01)00474-6

APA

Allahverdi, R., Enqvist, K., Mazumdar, A., & Pérez-Lorenzana, A. (2001). Baryogenesis in theories with large extra spatial dimensions. Nuclear Physics B, 618(1-2), 277-300. https://doi.org/10.1016/S0550-3213(01)00474-6

Vancouver

Allahverdi R, Enqvist K, Mazumdar A, Pérez-Lorenzana A. Baryogenesis in theories with large extra spatial dimensions. Nuclear Physics B. 2001 Dec 10;618(1-2):277-300. doi: 10.1016/S0550-3213(01)00474-6

Author

Allahverdi, Rouzbeh ; Enqvist, Kari ; Mazumdar, Anupam et al. / Baryogenesis in theories with large extra spatial dimensions. In: Nuclear Physics B. 2001 ; Vol. 618, No. 1-2. pp. 277-300.

Bibtex

@article{61ab66b8565f443e97c9f54877022108,
title = "Baryogenesis in theories with large extra spatial dimensions",
abstract = "We describe a simple and predictive scenario for baryogenesis in theories with large extra dimensions which resembles Affleck-Dine baryogenesis. The Affleck-Dine field is a complex scalar field carrying a $U(1)_{\chi}$ charge which is dynamically broken after the end of inflation. This generates an excess of $\chi$ over $\bar \chi$, which then decays into Standard Model fermions to produce an excess of baryons over anti-baryons. Our model is very constrained because the Affleck-Dine field has to be sufficiently flat during inflation. It is also a source for density fluctuations which can be tested in the coming satellite and balloon experiments.",
author = "Rouzbeh Allahverdi and Kari Enqvist and Anupam Mazumdar and Abdel P{\'e}rez-Lorenzana",
note = "LaTeX file, 24 pages, no figures",
year = "2001",
month = dec,
day = "10",
doi = "10.1016/S0550-3213(01)00474-6",
language = "English",
volume = "618",
pages = "277--300",
journal = "Nuclear Physics B",
issn = "0550-3213",
publisher = "ELSEVIER SCIENCE BV",
number = "1-2",

}

RIS

TY - JOUR

T1 - Baryogenesis in theories with large extra spatial dimensions

AU - Allahverdi, Rouzbeh

AU - Enqvist, Kari

AU - Mazumdar, Anupam

AU - Pérez-Lorenzana, Abdel

N1 - LaTeX file, 24 pages, no figures

PY - 2001/12/10

Y1 - 2001/12/10

N2 - We describe a simple and predictive scenario for baryogenesis in theories with large extra dimensions which resembles Affleck-Dine baryogenesis. The Affleck-Dine field is a complex scalar field carrying a $U(1)_{\chi}$ charge which is dynamically broken after the end of inflation. This generates an excess of $\chi$ over $\bar \chi$, which then decays into Standard Model fermions to produce an excess of baryons over anti-baryons. Our model is very constrained because the Affleck-Dine field has to be sufficiently flat during inflation. It is also a source for density fluctuations which can be tested in the coming satellite and balloon experiments.

AB - We describe a simple and predictive scenario for baryogenesis in theories with large extra dimensions which resembles Affleck-Dine baryogenesis. The Affleck-Dine field is a complex scalar field carrying a $U(1)_{\chi}$ charge which is dynamically broken after the end of inflation. This generates an excess of $\chi$ over $\bar \chi$, which then decays into Standard Model fermions to produce an excess of baryons over anti-baryons. Our model is very constrained because the Affleck-Dine field has to be sufficiently flat during inflation. It is also a source for density fluctuations which can be tested in the coming satellite and balloon experiments.

U2 - 10.1016/S0550-3213(01)00474-6

DO - 10.1016/S0550-3213(01)00474-6

M3 - Journal article

VL - 618

SP - 277

EP - 300

JO - Nuclear Physics B

JF - Nuclear Physics B

SN - 0550-3213

IS - 1-2

ER -