How to tell the shape of a wormhole by its quasinormal modes

Here we shall show how to reconstruct the shape function of a spherically symmetric traversable Lorenzian wormhole near its throat if one knows high frequency quasinormal modes of the wormhole. The wormhole spacetime is given by the Morris–Thorne ansatz. The solution to the inverse problem via fitting of the parameters within the WKB approach is unique for arbitrary tideless wormholes and some wormholes with non-zero tidal effects, but this is not so for arbitrary wormholes. As examples, we reproduce the near throat geometries of the Bronnikov–Ellis and tideless Morris–Thorne metrics by their quasinormal modes at high multipole numbers ℓ. © 2018

Авторы
Konoplya R.A. 1, 2, 3
Редакторы
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Издательство
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Номер выпуска
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Язык
Английский
Страницы
43-49
Статус
Опубликовано
Подразделение
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Номер
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Том
784
Год
2018
Организации
  • 1 Institute of Physics, Research Centre of Theoretical Physics and Astrophysics, Faculty of Philosophy and Science, Silesian University in Opava, Opava, CZ-746 01, Czech Republic
  • 2 Peoples Friendship University of Russia (RUDN University), 6 Miklukho-Maklaya Street, Moscow, 117198, Russian Federation
  • 3 Theoretical Astrophysics, Eberhard-Karls University of Tübingen, Tübingen, 72076, Germany
Ключевые слова
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Дата создания
19.10.2018
Дата изменения
19.10.2018
Постоянная ссылка
https://repository.rudn.ru/ru/records/article/record/6419/