@MastersThesis{Ladislau:2019:AnMePe,
author = "Ladislau, Samantha Monaliza",
title = "An{\'a}lises dos mecanismos de perda de energia e os
{\'{\i}}ndices de freamento em pulsares",
school = "Instituto Nacional de Pesquisas Espaciais (INPE)",
year = "2019",
address = "S{\~a}o Jos{\'e} dos Campos",
month = "2019-02-26",
keywords = "Estrela de n{\^e}utrons, pulsares, pulsares isolados, spindown,
{\'{\i}}ndice de frenagem, neutron stars, pulsars, isolated
pulsars, spindown, braking index.",
abstract = "Estrelas de n{\^e}utrons n{\~a}o-axissim{\'e}tricas e em
r{\'a}pida rota{\c{c}}{\~a}o s{\~a}o candidatas
prop{\'{\i}}cias a serem observadas pelos detectores Einstein
Telescope (ET) e Cosmic Explorer (CE) considerando limites
superiores de produ{\c{c}}{\~a}o de ondas gravitacionais
cont{\'{\i}}nuas por essas fontes. Entretanto, {\'e}
poss{\'{\i}}vel obter previs{\~o}es para a possibilidade de
detec{\c{c}}{\~a}o levando em conta outros mecanismos de perda
de energia em pulsares. Desde o final da d{\'e}cada de 1960,
temos conhecimento de que, embora os pulsares tenham seus
per{\'{\i}}odos de rota{\c{c}}{\~a}o muito est{\'a}veis, eles
n{\~a}o s{\~a}o constantes e apresentam varia{\c{c}}{\~o}es
entre ~ (10\−20\−10\−9) s s\−1. No
{\^a}mbito da pesquisa de spindown dos pulsares, v{\'a}rios
esfor{\c{c}}os t{\^e}m sido feitos para se entender o que leva
esses objetos a desacelerarem, bem como os {\'{\i}}ndices de
frenagem medidos. {\'E} nesse contexto que o presente trabalho
traz uma an{\'a}lise de combina{\c{c}}{\~o}es entre os modelos
de perda de energia por radia{\c{c}}{\~a}o de dipolo
magn{\'e}tico (RDM), por ondas gravitacionais (OGs), por Quantum
Vacuum Friction (QVF) e por vento de part{\'{\i}}culas (VP) e a
consequ{\^e}ncia dessas combina{\c{c}}{\~o}es na
evolu{\c{c}}{\~a}o do {\^a}ngulo de inclina{\c{c}}{\~a}o
magn{\'e}tica (ø) do pulsar, na sua velocidade angular (omega) e
no {\'{\i}}ndice de frenagem (n). Mostramos que tanto QVF como
VP combinados {\`a} RDM s{\~a}o capazes de explicar o menor
{\'{\i}}ndice de frenagem j{\'a} medido n = 0, 9 ± 0, 2, para o
pulsar PSR J1734-3333. Al{\'e}m disso, mostramos como {\'e} a
evolu{\c{c}}{\~a}o acoplada entre rota{\c{c}}{\~a}o e o
{\^a}ngulo de inclina{\c{c}}{\~a}o magn{\'e}tica e
conclu{\'{\i}}mos que o QVF {\'e} respons{\'a}vel por atrasar
o alinhamento do pulsar. Adicionalmente, investigamos como
diferentes valores de massa em pulsares alimentados por
rota{\c{c}}{\~a}o e o movimento de precess{\~a}o influenciam a
amplitude das OGs geradas por tais objetos e qual o potencial de
detec{\c{c}}{\~a}o dessas fontes pela nova gera{\c{c}}{\~a}o
de detectores de OGs. Como resultado, obtivemos que, mesmo numa
perspectiva otimista, considerando pulsares com massas ~ 2,0 M.,
essas fontes n{\~a}o seriam detectadas pelo aLIGO se a
deforma{\c{c}}{\~a}o do pulsar for de origem magn{\'e}tica.
J{\'a} no modelo de gera{\c{c}}{\~a}o de OGs por movimento de
precess{\~a}o, obtivemos que em um tempo de
integra{\c{c}}{\~a}o de 1 ano os pulsares Vela e Caranguejo
seriam detectados pelo ET e pelo CE se as ENs tiverem (epsilon) ~~
10\−5 e wobble angle (alpha) = 0, 1 rad. ABSTRACT:
Non-axisymmetric and fast-spinning neutron stars are suitable
candidates to be observed by the detectors Einstein Telescope (ET)
and Cosmic Explorer (CE) considering upper limits of continuous
gravitational waves production by these sources. However, it is
possible to obtain predictions for the possibility of detection
taking into account other mechanisms of loss of energy in pulsars.
Since the late 1960s, we have learned that although pulsars have
very stable rotation periods, they are not constant and vary (~
10\−20 \− 10\−9 s s\−1) . In the scope
of pulsar spindown research, several efforts have been made to
understand what causes these objects to decelerate, as well as the
measured braking indices. In this context the present work brings
an analysis of combinations between the energy loss models by
magnetic dipole radiation (MDR), gravitational waves (GW), quantum
vacuum friction (QVF) and particle wind (PW) and the consequence
of these combinations on the evolution of the magnetic inclination
angle ø, angular velocity and the braking index n. We show that
both QVF and PW combined with MDR are able to explain the lowest
measured braking index (n = 0.9 ± 0.2) for PSR J1734-3333. In
addition, we show the coupled evolution between rotation and
magnetic inclination angle and we conclude that the QVF is
responsible for delaying the alignment of the pulsar.
Additionally, we investigated the effect of different mass values
of rotation powered pulsar (RPP) on the the amplitude of the GW
and we study the possibility of GW generated by RPPs precession
motion being detected by new generation of gravitational wave
detectors. As a result, we obtained that, even in an optimistic
perspective, considering pulsars with masses of 2.0 solar masses,
these sources would not be detected by the aLIGO if the pulsar
deformation is of magnetic origin. In the model of GW generated by
precession motion, we concluded that Vela and Crab pulsars would
be detect in one year of integration by ET and EC with (epsilon)
~~ 10\−5 and wobble angle (alpha) = 0.1 rad.",
committee = "Aguiar, Odylio Denys de (presidente) and Ara{\'u}jo, Jos{\'e}
Carlos Neves de (orientador) and Coelho, Jaziel Goulart
(orientador) and Rodrigues, Cl{\'a}udia Vilega and
Magalh{\~a}es, Nadja Sim{\~a}o",
englishtitle = "Analysis of energy loss mechanisms and pulsars braking indices",
language = "pt",
pages = "99",
ibi = "8JMKD3MGP3W34R/3SNU35H",
url = "http://urlib.net/ibi/8JMKD3MGP3W34R/3SNU35H",
targetfile = "publicacao.pdf",
urlaccessdate = "26 abr. 2024"
}