Abstract
We present a brief history of the field and the reasons which motivate such an enterprise, starting from the concept of asteroseismology and how it can be applied in neutron stars, so that the equation of state of dense nuclear matter is determined. Then, we discuss neutron stars as gravitational-wave sources, focusing on the presence of unstable oscillation modes and reviewing their significance both for gravitational-wave asteroseismology and neutron star evolution.
You will smile and hold my hands tight.
A star will ring on the damp sky.
I may
cry.
Tasos Livaditis, Simple talk (1950)
English translation: P. P.
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Notes
- 1.
Five spheres for the planets known at the time (Mercury, Venus, Mars, Jupiter, Saturn), two spheres for the Sun and Moon, plus one for the distant stars.
- 2.
The Republic of Plato, X617b. Translated by Allan Bloom. New York: Basic Books, 2nd ed. (1991).
- 3.
T
\(\Lambda \) 
, ‘A\(\pi \lambda \tilde{\eta }\ \kappa ov\beta \acute{\varepsilon }\nu \tau a\) (M
, 1950). \(\varPi o\acute{\iota }\eta \sigma \eta \), T
105. A
: K
(2002).
, ‘A
, 1950). 
105. A
: K
(2002).References
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Pnigouras, P. (2018). Introduction. In: Saturation of the f-mode Instability in Neutron Stars. Springer Theses. Springer, Cham. https://doi.org/10.1007/978-3-319-98258-8_1
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