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dc.contributor.author | Transtromer, G | en |
dc.contributor.author | Treille, D | en |
dc.contributor.author | Tristram, G | en |
dc.contributor.author | Trombini, A | en |
dc.contributor.author | Troncon, C | en |
dc.contributor.author | Tsirou, A | en |
dc.contributor.author | Turluer, M-L | en |
dc.contributor.author | Tyapkin, IA | en |
dc.contributor.author | Tyndel, M | en |
dc.contributor.author | Tzamarias, S | en |
dc.contributor.author | Ueberschaer, B | en |
dc.contributor.author | Ullaland, O | en |
dc.contributor.author | Uvarov, V | en |
dc.contributor.author | Valenti, G | en |
dc.contributor.author | Vallazza, E | en |
dc.contributor.author | Vander Velde, C | en |
dc.contributor.author | van Apeldoorn, GW | en |
dc.contributor.author | van Dam, P | en |
dc.contributor.author | van Doninck, WK | en |
dc.contributor.author | van Eldik, J | en |
dc.contributor.author | van Lysebetten, A | en |
dc.contributor.author | Vassilopoulos, N | en |
dc.contributor.author | Vegni, G | en |
dc.contributor.author | Ventura, L | en |
dc.contributor.author | Venus, W | en |
dc.contributor.author | Verbeure, F | en |
dc.contributor.author | Verlato, M | en |
dc.contributor.author | Vertogradov, LS | en |
dc.contributor.author | Vilanova, D | en |
dc.contributor.author | Vincent, P | en |
dc.contributor.author | Vitale, L | en |
dc.contributor.author | Vlasov, E | en |
dc.contributor.author | Vodopyanov, AS | en |
dc.contributor.author | Vrba, V | en |
dc.contributor.author | Wahlen, H | en |
dc.contributor.author | Walck, C | en |
dc.contributor.author | Waldner, F | en |
dc.contributor.author | Weiser, C | en |
dc.contributor.author | Wetherell, AM | en |
dc.contributor.author | Wicke, D | en |
dc.contributor.author | Wickens, JH | en |
dc.contributor.author | Wielers, M | en |
dc.contributor.author | Wilkinson, GR | en |
dc.contributor.author | Williams, WSC | en |
dc.contributor.author | Winter, M | en |
dc.contributor.author | Witek, M | en |
dc.contributor.author | Wlodek, T | en |
dc.contributor.author | Yi, J | en |
dc.contributor.author | Yip, K | en |
dc.contributor.author | Yushchenko, O | en |
dc.contributor.author | Zach, F | en |
dc.contributor.author | Zaitsev, A | en |
dc.contributor.author | Zalewska, A | en |
dc.contributor.author | Zalewski, P | en |
dc.contributor.author | Zavrtanik, D | en |
dc.contributor.author | Zevgolatakos, E | en |
dc.contributor.author | Zimin, NI | en |
dc.contributor.author | Zucchelli, GC | en |
dc.contributor.author | Zumerle, G | en |
dc.date.accessioned | 2014-03-01T01:47:27Z | |
dc.date.available | 2014-03-01T01:47:27Z | |
dc.date.issued | 1998 | en |
dc.identifier.issn | 14346044 | en |
dc.identifier.uri | https://dspace.lib.ntua.gr/xmlui/handle/123456789/25217 | |
dc.relation.uri | http://www.scopus.com/inward/record.url?eid=2-s2.0-0006556017&partnerID=40&md5=cc471bad9b90b05682e17b316d6f1d5c | en |
dc.title | Search for charginos, neutralinos and gravitinos at LEP | en |
heal.type | journalArticle | en |
heal.publicationDate | 1998 | en |
heal.abstract | An update of the searches for charginos and neutralinos in DELPHI is presented, based mainly on recent data collected at centre-of-mass energies of 161 GeV and 172 GeV. No signal is found. For a sneutrino with mass above 300 GeV/c2 and a mass difference between the chargino and the lightest neutralino above 10 GeV/c2, the lower limit at 95% confidence level on the chargino mass ranges from 84.3 GeV/c2 to the kinematical limit (86.0 GeV/c2), depending on the mixing parameters. The limit decreases for lower chargino-neutralino mass differences. The limit in the case of a light sneutrino is 67.6 GeV/c2, provided that that there is no light sneutrino with a mass within 10 GeV/c2 below the chargino mass. Upper limits on neutralino pair production cross-sections of about a picobarn are derived. The (μ, M2) domain excluded in the MSSM-GUT scenario is determined by combining the neutralino and chargino searches. These results imply a limit on the mass of the lightest neutralino which, for a heavy sneutrino, is constrained to be above 24.9 GeV/c2 for tanβ ≥ 1. The search has also been extended to the case where the lightest neutralino is unstable and decays into a photon and a gravitino. | en |
heal.journalName | European Physical Journal C | en |
dc.identifier.volume | 1 | en |
dc.identifier.issue | 1-2 | en |
dc.identifier.spage | 1 | en |
dc.identifier.epage | 20 | en |
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