語系:
繁體中文
English
說明(常見問題)
登入
回首頁
切換:
標籤
|
MARC模式
|
ISBD
Saturation of the f-mode instability...
~
Pnigouras, Pantelis.
Saturation of the f-mode instability in neutron stars
紀錄類型:
書目-語言資料,印刷品 : Monograph/item
正題名/作者:
Saturation of the f-mode instability in neutron stars/ by Pantelis Pnigouras.
作者:
Pnigouras, Pantelis.
出版者:
Cham :Springer International Publishing : : 2018.,
面頁冊數:
xxiii, 220 p. :ill., digital ; : 24 cm.;
Contained By:
Springer eBooks
標題:
Neutron stars. -
電子資源:
https://doi.org/10.1007/978-3-319-98258-8
ISBN:
9783319982588
Saturation of the f-mode instability in neutron stars
Pnigouras, Pantelis.
Saturation of the f-mode instability in neutron stars
[electronic resource] /by Pantelis Pnigouras. - Cham :Springer International Publishing :2018. - xxiii, 220 p. :ill., digital ;24 cm. - Springer theses,2190-5053. - Springer theses..
Introduction -- The Oscillation Modes: Linear Perturbation Scheme -- The f-mode Instability -- Mode Coupling: Quadratic Perturbation Scheme -- Results -- Final Remarks.
This book presents a study of the saturation of unstable f-modes (fundamental modes) due to low-order nonlinear mode coupling. Since their theoretical prediction in 1934, neutron stars have remained among the most challenging objects in the Universe. Gravitational waves emitted by unstable neutron star oscillations can be used to obtain information about their inner structure, that is, the equation of state of dense nuclear matter. After its initial growth phase, the instability is expected to saturate due to nonlinear effects. The saturation amplitude of the unstable mode determines the detectability of the generated gravitational-wave signal, but also affects the evolution of the neutron star. The study shows that the unstable (parent) mode resonantly couples to pairs of stable (daughter) modes, which drain the parent's energy and make it saturate via a mechanism called parametric resonance instability. Further, it calculates the saturation amplitude of the most unstable f-mode multipoles throughout their so-called instability windows.
ISBN: 9783319982588
Standard No.: 10.1007/978-3-319-98258-8doiSubjects--Topical Terms:
672991
Neutron stars.
LC Class. No.: QB843.N4 / P554 2018
Dewey Class. No.: 523.8874
Saturation of the f-mode instability in neutron stars
LDR
:02267nam a2200349 a 4500
001
929281
003
DE-He213
005
20190318134911.0
006
m d
007
cr nn 008maaau
008
190626s2018 gw s 0 eng d
020
$a
9783319982588
$q
(electronic bk.)
020
$a
9783319982571
$q
(paper)
024
7
$a
10.1007/978-3-319-98258-8
$2
doi
035
$a
978-3-319-98258-8
040
$a
GP
$c
GP
041
0
$a
eng
050
4
$a
QB843.N4
$b
P554 2018
072
7
$a
PGC
$2
bicssc
072
7
$a
SCI004000
$2
bisacsh
072
7
$a
PGC
$2
thema
072
7
$a
PHVB
$2
thema
082
0 4
$a
523.8874
$2
23
090
$a
QB843.N4
$b
P738 2018
100
1
$a
Pnigouras, Pantelis.
$3
1209712
245
1 0
$a
Saturation of the f-mode instability in neutron stars
$h
[electronic resource] /
$c
by Pantelis Pnigouras.
260
$a
Cham :
$c
2018.
$b
Springer International Publishing :
$b
Imprint: Springer,
300
$a
xxiii, 220 p. :
$b
ill., digital ;
$c
24 cm.
490
1
$a
Springer theses,
$x
2190-5053
505
0
$a
Introduction -- The Oscillation Modes: Linear Perturbation Scheme -- The f-mode Instability -- Mode Coupling: Quadratic Perturbation Scheme -- Results -- Final Remarks.
520
$a
This book presents a study of the saturation of unstable f-modes (fundamental modes) due to low-order nonlinear mode coupling. Since their theoretical prediction in 1934, neutron stars have remained among the most challenging objects in the Universe. Gravitational waves emitted by unstable neutron star oscillations can be used to obtain information about their inner structure, that is, the equation of state of dense nuclear matter. After its initial growth phase, the instability is expected to saturate due to nonlinear effects. The saturation amplitude of the unstable mode determines the detectability of the generated gravitational-wave signal, but also affects the evolution of the neutron star. The study shows that the unstable (parent) mode resonantly couples to pairs of stable (daughter) modes, which drain the parent's energy and make it saturate via a mechanism called parametric resonance instability. Further, it calculates the saturation amplitude of the most unstable f-mode multipoles throughout their so-called instability windows.
650
0
$a
Neutron stars.
$3
672991
650
1 4
$a
Theoretical Astrophysics.
$3
1207848
650
2 4
$a
Astrophysics and Astroparticles.
$3
782546
710
2
$a
SpringerLink (Online service)
$3
593884
773
0
$t
Springer eBooks
830
0
$a
Springer theses.
$3
831604
856
4 0
$u
https://doi.org/10.1007/978-3-319-98258-8
950
$a
Physics and Astronomy (Springer-11651)
筆 0 讀者評論
多媒體
評論
新增評論
分享你的心得
Export
取書館別
處理中
...
變更密碼[密碼必須為2種組合(英文和數字)及長度為10碼以上]
登入