Skip to Main Content

Access Provided by Xinjiang University

Physical Review D

Access by Xinjiang University

Higgs decays in supersymmetric models with light neutralinos

Carlos E. Yaguna^*

Department of Physics and Astronomy, UCLA, Portola Plaza, Los Angeles, California 90095, USA

^*yaguna@physics.ucla.edu

Phys. Rev. D 76, 075017 – Published 30 October, 2007

DOI: https://doi.org/10.1103/PhysRevD.76.075017

Abstract

In the minimal supersymmetric standard model, neutralinos lighter than 50 GeV are compatible with all accelerator, precision, and cosmological bounds. Such neutralinos might constitute a relevant decay channel for the Higgs boson, modifying its expected signatures at hadron colliders. We study the branching ratio $h \to χ χ$ and determine the region in the supersymmetric parameter space where it is significant. We have found that, in fact, the Higgs may dominantly decay into neutralino pairs. Besides, as a result of this new channel, the branching ratio into visible modes, such as $h \to γ γ$ , gets suppressed.

Article Text

References (21)

R. Barate et al. (LEP Working Group for Higgs Boson Ssearches), Phys. Lett. B 565, 61 (2003) [arXiv:hep-ex/0306033].
ALEPH Collaboration, Phys. Rep. 427, 257 (2006) [arXiv:hep-ex/0509008]; ALEPH Collaboration, arXiv:hep-ex/0511027.
W. M. Yao et al. (Particle Data Group), J. Phys. G 33, 1 (2006).
C. T. Hill, Phys. Lett. B 135, 47 (1984); J. R. Ellis, K. Enqvist, D. V. Nanopoulos, and K. Tamvakis, 155, 381 (1985); M. Drees, 158, 409 (1985); G. Anderson, C. H. Chen, J. F. Gunion, J. D. Lykken, T. Moroi, and Y. Yamada, arXiv:hep-ph/9609457; K. Huitu, Y. Kawamura, T. Kobayashi, and K. Puolamaki, Phys. Rev. D 61, 035001 (1999) [arXiv:hep-ph/9903528]; U. Chattopadhyay and D. P. Roy, 68, 033010 (2003) [arXiv:hep-ph/0304108]; S. Profumo and C. E. Yaguna, Nucl. Phys. B681, 247 (2004) [arXiv:hep-ph/0307225].
H. K. Dreiner, S. Heinemeyer, O. Kittel, U. Langenfeld, A. M. Weber, and G. Weiglein, arXiv:0707.1425.
D. N. Spergel et al. (WMAP Collaboration), Astrophys. J. Suppl. Ser. 170, 377 (2007) [arXiv:astro-ph/0603449].
D. Hooper and T. Plehn, Phys. Lett. B 562, 18 (2003) [arXiv:hep-ph/0212226]; A. Bottino, N. Fornengo, and S. Scopel, Phys. Rev. D 67, 063519 (2003) [arXiv:hep-ph/0212379]; A. Bottino, F. Donato, N. Fornengo, and S. Scopel, 69, 037302 (2004) [arXiv:hep- ph/0307303]; G. Belanger, F. Boudjema, A. Cottrant, A. Pukhov, and S. Rosier-Lees, J. High Energy Phys. 03 (2004) 012 [arXiv:hep-ph/0310037]. A. Bottino, F. Donato, N. Fornengo, and S. Scopel, Phys. Rev. D 70, 015005 (2004) [arXiv:hep-ph/0401186]; A. Bottino, F. Donato, N. Fornengo, and P. Salati, 72, 083518 (2005) [arXiv:hep-ph/0507086]; A. Bottino, F. Donato, N. Fornengo, and S. Scopel, 72, 083521 (2005) [arXiv:hep-ph/0508270]; J. S. Lee and S. Scopel, 75, 075001 (2007) [arXiv:hep-ph/0701221].
G. B. Gelmini, P. Gondolo, A. Soldatenko, and C. E. Yaguna, Phys. Rev. D 76, 015010 (2007) [arXiv:hep-ph/0610379].
S. G. Frederiksen, N. Johnson, G. L. Kane, and J. Reid, Phys. Rev. D 50, R4244 (1994); S. P. Martin and J. D. Wells, 60, 035006 (1999) [arXiv:hep-ph/9903259].
R. M. Godbole, M. Guchait, K. Mazumdar, S. Moretti, and D. P. Roy, Phys. Lett. B 571, 184 (2003) [arXiv:hep-ph/0304137].
H. Davoudiasl, T. Han, and H. E. Logan, Phys. Rev. D 71, 115007 (2005) [arXiv:hep- ph/0412269].
G. Belanger, F. Boudjema, F. Donato, R. Godbole, and S. Rosier-Lees, Nucl. Phys. B581, 3 (2000) [arXiv:hep-ph/0002039].
G. Belanger, F. Boudjema, A. Cottrant, R. M. Godbole, and A. Semenov, Phys. Lett. B 519, 93 (2001) [arXiv:hep-ph/0106275].
T. Moroi, M. Yamaguchi, and T. Yanagida, Phys. Lett. B 342, 105 (1995); M. Kawasaki, T. Moroi, and T. Yanagida, 370, 52 (1996); T. Moroi and L. Randall, Nucl. Phys. B570, 455 (2000); M. Fujii and K. Hamaguchi, Phys. Rev. D 66, 083501 (2002); M. Fujii and M. Ibe, 69, 035006 (2004); D. H. Lyth and E. D. Stewart, 53, 1784 (1996); M. Kamionkowski and M. S. Turner, 42, 3310 (1990); J. D. Barrow, Nucl. Phys. B208, 501 (1982); P. Salati, Phys. Lett. B 571, 121 (2003) [arXiv:astro-ph/0207396]; S. Profumo and P. Ullio, J. Cosmol. Astropart. Phys. 11 (2003) 006 [arXiv:hep-ph/0309220]; G. Gelmini, P. Gondolo, A. Soldatenko, and C. E. Yaguna, Phys. Rev. D 74, 083514 (2006) [arXiv:hep-ph/0605016].
L. Reina, arXiv:hep-ph/0512377.
A. Djouadi, arXiv:hep-ph/0503173.
M. Davier, Nucl. Phys. B, Proc. Suppl. 169, 288 (2007) [arXiv:hep-ph/0701163].
E. Barberio et al. (Heavy Flavor Averaging Group (HFAG)), arXiv:hep-ex/0603003.
T. Hahn, S. Heinemeyer, W. Hollik, H. Rzehak, G. Weiglein, and K. Williams, arXiv:hep-ph/0611373; G. Degrassi, S. Heinemeyer, W. Hollik, P. Slavich, and G. Weiglein, Eur. Phys. J. C 28, 133 (2003) [arXiv:hep-ph/0212020]; S. Heinemeyer, W. Hollik, and G. Weiglein, Comput. Phys. Commun. 124, 76 (2000) [arXiv:hep-ph/9812320]; Eur. Phys. J. C 9, 343 (1999) [arXiv:hep-ph/9812472].
A. Djouadi, M. Drees, P. Fileviez Perez, and M. Muhlleitner, Phys. Rev. D 65, 075016 (2002) [arXiv:hep-ph/0109283].
Since $BR (h \to χ χ)$ depends also on $\tan β$ , the suppression will depend on $\tan β$ too.