2.5 Méthodes de gestion pour les PME
2.5.1 Mehari Pro
Os modelos expansionistas teóricos que apresentam histórias similares, mas pos- suem parâmetros diferentes para caracterizar a expansão, podem, através do parâmetro γ, ser diferenciados observacionalmente através dos desvios no plano teórico compreen- didos em seu significado; em outras palavras, modelos cosmológicos com história da ex- pansão idênticas, mas construidas em teorias gravitacionais diferentes, devem apresentar valores de γ também diferentes.
Desse modo, um estudo complementar e que poderá mostrar resultados interes- santes, é analisar as medidas da velocidade peculiar de galáxias para obter restrições sobre possíveis modificações na Relatividade Geral. Tentativas nessa direção podem ser encon- tradas nas referências [244, 245].
É possível analisarmos o processo de formação de estruturas usando o modelo padrão de Press & Schechter e a evolução de flutuações de densidade primordiais nesse formalismo [246]. Dentro desse contexto, uma região compreendida por uma flutuação de matéria δ, ou um campo eleatório P (δM)descrito por uma distribuição gaussiana [157,
2, 246] tornar-se-a um objeto auto-gravitante quando ela alcança um certo valor crítico δc,
significando que essa flutuação evoluiu e destacou-se da expansão de Hubble de maneira a se transformar em um objeto gravitacional ligado.
A isso aplicaremos os diferentes modelos de energia escura descritos e os com- pararemos com os resultados do modelo padrão ΛCDM, o que nos permitirá entender a influência do modelo de Press & Schechter na evolução das flutuações de densidade quando o compararmos com os resultados modelados no perfil Top-Hat.
Os fundamentos da Termodinâmica e da Mecânica Estatística vem apresentando desde as últimas décadas interessantes discussões sobre a aditividade e não-aditividade
Capítulo 9. Conclusões e perspectivas futuras 113
dos parâmetros presentes nos processos físicos ocorrentes em seus arcabouços teóricos, inicialmente tomados pelos estudos pioneiros de Tsallis e Kaniadakis [247, 248].
Atualmente vem sendo observado um interesse significativo na estatística de Tsal- lis e suas aplicações na Cosmologia e Astrofísica, principalmente a partir do trabalho de A. R. Plastino & A. Plastino [249]. Nesse contexto, as propriedades termodinâmicas apre- sentam modificações significativas devido à interações de longo alcance como no caso das forças gravitacionais [250, 251, 252]. Diversas outras aplicações podem ser encontradas nas referências [253, 254, 255, 256, 257, 258].
O estudo dessa estatística é amplo e rico em sua estrutura física. Abordagens so- bre essa estatística cobrem a análise de teorias não-aditivas da matéria escura e a estrutura dos perfis de densidade dos gases [259] e indícios de que as flutuações de temperatura da RCF corresponderiam a uma natureza não-aditiva [260]. Desse modo, seria natural um interesse em aplicarmos a estatística não-aditiva de Tsallis para descrevermos o processo de formação de estruturas no Universo.
Não menos interessante seria uma análise complementar sobre a distribuição de Kaniadakis [248, 261] e suas implicações no estudo do campo primordial das flutuações de densidade. Assim como no estudo de Tsallis, a estatística de Kaniadakis recupera o formalismo de Boltzmann-Gibbs para um determinado valor de κ que caracteriza a pa- rametrização da distribuição de Kaniadakis, que diferentemente da estatística de Tsallis, continua numa contextualização aditiva sobre os parâmetros que participam dos proces- sos físicos envolvidos.
Investigaremos o processo de formação de estruturas e analisaremos os métodos Top-Hate Press & Schechter no formalismo não-aditivo de Tsallis e na formulação estatís- tica de Kaniadakis na presença das componentes escuras (matéria e energia) de modo que possamos computar a influência dessas componentes nesse processo.
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