Exploring a search for long-duration transient gravitational waves associated with magnetar bursts

Ryan Quitzow-James, James E Brau, James A. Clark, Michael W Coughlin, Scott B Coughlin, Raymond Frey, Paul Schale, Dipongkar Talukder, Eric Thrane

Research output: Contribution to journalArticleResearchpeer-review

2 Citations (Scopus)

Abstract

Soft gamma repeaters and anomalous x-ray pulsars are thought to be magnetars, neutron stars with strong magnetic fields of order $ \newcommand{\unsim}{\mathord{\sim}} \unsim$ $ 10^{13}$ –$ \newcommand{\gauss}{{\rm gauss}} 10^{15} \gauss$ . These objects emit intermittent bursts of hard x-rays and soft gamma rays. Quasiperiodic oscillations in the x-ray tails of giant flares imply the existence of neutron star oscillation modes which could emit gravitational waves powered by the magnetar's magnetic energy reservoir. We describe a method to search for transient gravitational-wave signals associated with magnetar bursts with durations of 10 s to 1000 s of seconds. The sensitivity of this method is estimated by adding simulated waveforms to data from the sixth science run of Laser Interferometer Gravitational-wave Observatory (LIGO). We find a search sensitivity in terms of the root sum square strain amplitude of $ \newcommand{\hertz}{{\rm Hz}} \newcommand{\hrss}{h_{\rm rss}} \newcommand{\h}{\mathfrak{h}} \hrss = 1.3 \times 10^{-21}~\hertz^{-1/2}$ for a half sine-Gaussian waveform with a central frequency $f_0 = 150$ Hz and a characteristic time $\tau = 400$ s. This corresponds to a gravitational wave energy of $ \newcommand{\erg}{{\rm erg}} \newcommand{\ergs}{\erg} \newcommand{\EGW}{E_{\rm GW}} \EGW = 4.3 \times 10^{46}~{\rm \ergs}$ , the same order of magnitude as the 2004 giant flare which had an estimated electromagnetic energy of $ \newcommand{\unsim}{\mathord{\sim}} \newcommand{\erg}{{\rm erg}} \newcommand{\ergs}{\erg} \newcommand{\EEM}{E_{\rm EM}} \newcommand{\h}{\mathfrak{h}} \EEM = \unsim 1.7 \times 10^{46} (d/ 8.7~{\rm kpc}){\hspace{0pt}}^2~{\rm \ergs}$ , where d is the distance to SGR 1806-20. We present an extrapolation of these results to Advanced LIGO, estimating a sensitivity to a gravitational wave energy of $ \newcommand{\erg}{{\rm erg}} \newcommand{\ergs}{\erg} \newcommand{\EGW}{E_{\rm GW}} \newcommand{\bestUL}{4.3 \times 10^{46}} \newcommand{\bestULaLIGO}{9.0 \times 10^{44}} \newcommand{\bestULaLIGOclose}{3.2 \times 10^{43}} \EGW = \bestULaLIGOclose~{\rm \ergs}$ for a magnetar at a distance of $1.6$ kpc. These results suggest this search method can probe significantly below the energy budgets for magnetar burst emission mechanisms such as crust cracking and hydrodynamic deformation.
Original languageEnglish
Article number164002
Number of pages16
JournalClassical and Quantum Gravity
Volume34
Issue number16
DOIs
Publication statusPublished - 20 Jul 2017

Keywords

  • data analysis
  • gravitational waves
  • magnetars

Cite this

Quitzow-James, Ryan ; Brau, James E ; Clark, James A. ; Coughlin, Michael W ; Coughlin, Scott B ; Frey, Raymond ; Schale, Paul ; Talukder, Dipongkar ; Thrane, Eric. / Exploring a search for long-duration transient gravitational waves associated with magnetar bursts. In: Classical and Quantum Gravity. 2017 ; Vol. 34, No. 16.
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abstract = "Soft gamma repeaters and anomalous x-ray pulsars are thought to be magnetars, neutron stars with strong magnetic fields of order $ \newcommand{\unsim}{\mathord{\sim}} \unsim$ $ 10^{13}$ –$ \newcommand{\gauss}{{\rm gauss}} 10^{15} \gauss$ . These objects emit intermittent bursts of hard x-rays and soft gamma rays. Quasiperiodic oscillations in the x-ray tails of giant flares imply the existence of neutron star oscillation modes which could emit gravitational waves powered by the magnetar's magnetic energy reservoir. We describe a method to search for transient gravitational-wave signals associated with magnetar bursts with durations of 10 s to 1000 s of seconds. The sensitivity of this method is estimated by adding simulated waveforms to data from the sixth science run of Laser Interferometer Gravitational-wave Observatory (LIGO). We find a search sensitivity in terms of the root sum square strain amplitude of $ \newcommand{\hertz}{{\rm Hz}} \newcommand{\hrss}{h_{\rm rss}} \newcommand{\h}{\mathfrak{h}} \hrss = 1.3 \times 10^{-21}~\hertz^{-1/2}$ for a half sine-Gaussian waveform with a central frequency $f_0 = 150$ Hz and a characteristic time $\tau = 400$ s. This corresponds to a gravitational wave energy of $ \newcommand{\erg}{{\rm erg}} \newcommand{\ergs}{\erg} \newcommand{\EGW}{E_{\rm GW}} \EGW = 4.3 \times 10^{46}~{\rm \ergs}$ , the same order of magnitude as the 2004 giant flare which had an estimated electromagnetic energy of $ \newcommand{\unsim}{\mathord{\sim}} \newcommand{\erg}{{\rm erg}} \newcommand{\ergs}{\erg} \newcommand{\EEM}{E_{\rm EM}} \newcommand{\h}{\mathfrak{h}} \EEM = \unsim 1.7 \times 10^{46} (d/ 8.7~{\rm kpc}){\hspace{0pt}}^2~{\rm \ergs}$ , where d is the distance to SGR 1806-20. We present an extrapolation of these results to Advanced LIGO, estimating a sensitivity to a gravitational wave energy of $ \newcommand{\erg}{{\rm erg}} \newcommand{\ergs}{\erg} \newcommand{\EGW}{E_{\rm GW}} \newcommand{\bestUL}{4.3 \times 10^{46}} \newcommand{\bestULaLIGO}{9.0 \times 10^{44}} \newcommand{\bestULaLIGOclose}{3.2 \times 10^{43}} \EGW = \bestULaLIGOclose~{\rm \ergs}$ for a magnetar at a distance of $1.6$ kpc. These results suggest this search method can probe significantly below the energy budgets for magnetar burst emission mechanisms such as crust cracking and hydrodynamic deformation.",
keywords = "data analysis, gravitational waves, magnetars",
author = "Ryan Quitzow-James and Brau, {James E} and Clark, {James A.} and Coughlin, {Michael W} and Coughlin, {Scott B} and Raymond Frey and Paul Schale and Dipongkar Talukder and Eric Thrane",
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Quitzow-James, R, Brau, JE, Clark, JA, Coughlin, MW, Coughlin, SB, Frey, R, Schale, P, Talukder, D & Thrane, E 2017, 'Exploring a search for long-duration transient gravitational waves associated with magnetar bursts', Classical and Quantum Gravity, vol. 34, no. 16, 164002. https://doi.org/10.1088/1361-6382/aa7d5b

Exploring a search for long-duration transient gravitational waves associated with magnetar bursts. / Quitzow-James, Ryan; Brau, James E; Clark, James A.; Coughlin, Michael W; Coughlin, Scott B; Frey, Raymond; Schale, Paul; Talukder, Dipongkar; Thrane, Eric.

In: Classical and Quantum Gravity, Vol. 34, No. 16, 164002, 20.07.2017.

Research output: Contribution to journalArticleResearchpeer-review

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T1 - Exploring a search for long-duration transient gravitational waves associated with magnetar bursts

AU - Quitzow-James, Ryan

AU - Brau, James E

AU - Clark, James A.

AU - Coughlin, Michael W

AU - Coughlin, Scott B

AU - Frey, Raymond

AU - Schale, Paul

AU - Talukder, Dipongkar

AU - Thrane, Eric

PY - 2017/7/20

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N2 - Soft gamma repeaters and anomalous x-ray pulsars are thought to be magnetars, neutron stars with strong magnetic fields of order $ \newcommand{\unsim}{\mathord{\sim}} \unsim$ $ 10^{13}$ –$ \newcommand{\gauss}{{\rm gauss}} 10^{15} \gauss$ . These objects emit intermittent bursts of hard x-rays and soft gamma rays. Quasiperiodic oscillations in the x-ray tails of giant flares imply the existence of neutron star oscillation modes which could emit gravitational waves powered by the magnetar's magnetic energy reservoir. We describe a method to search for transient gravitational-wave signals associated with magnetar bursts with durations of 10 s to 1000 s of seconds. The sensitivity of this method is estimated by adding simulated waveforms to data from the sixth science run of Laser Interferometer Gravitational-wave Observatory (LIGO). We find a search sensitivity in terms of the root sum square strain amplitude of $ \newcommand{\hertz}{{\rm Hz}} \newcommand{\hrss}{h_{\rm rss}} \newcommand{\h}{\mathfrak{h}} \hrss = 1.3 \times 10^{-21}~\hertz^{-1/2}$ for a half sine-Gaussian waveform with a central frequency $f_0 = 150$ Hz and a characteristic time $\tau = 400$ s. This corresponds to a gravitational wave energy of $ \newcommand{\erg}{{\rm erg}} \newcommand{\ergs}{\erg} \newcommand{\EGW}{E_{\rm GW}} \EGW = 4.3 \times 10^{46}~{\rm \ergs}$ , the same order of magnitude as the 2004 giant flare which had an estimated electromagnetic energy of $ \newcommand{\unsim}{\mathord{\sim}} \newcommand{\erg}{{\rm erg}} \newcommand{\ergs}{\erg} \newcommand{\EEM}{E_{\rm EM}} \newcommand{\h}{\mathfrak{h}} \EEM = \unsim 1.7 \times 10^{46} (d/ 8.7~{\rm kpc}){\hspace{0pt}}^2~{\rm \ergs}$ , where d is the distance to SGR 1806-20. We present an extrapolation of these results to Advanced LIGO, estimating a sensitivity to a gravitational wave energy of $ \newcommand{\erg}{{\rm erg}} \newcommand{\ergs}{\erg} \newcommand{\EGW}{E_{\rm GW}} \newcommand{\bestUL}{4.3 \times 10^{46}} \newcommand{\bestULaLIGO}{9.0 \times 10^{44}} \newcommand{\bestULaLIGOclose}{3.2 \times 10^{43}} \EGW = \bestULaLIGOclose~{\rm \ergs}$ for a magnetar at a distance of $1.6$ kpc. These results suggest this search method can probe significantly below the energy budgets for magnetar burst emission mechanisms such as crust cracking and hydrodynamic deformation.

AB - Soft gamma repeaters and anomalous x-ray pulsars are thought to be magnetars, neutron stars with strong magnetic fields of order $ \newcommand{\unsim}{\mathord{\sim}} \unsim$ $ 10^{13}$ –$ \newcommand{\gauss}{{\rm gauss}} 10^{15} \gauss$ . These objects emit intermittent bursts of hard x-rays and soft gamma rays. Quasiperiodic oscillations in the x-ray tails of giant flares imply the existence of neutron star oscillation modes which could emit gravitational waves powered by the magnetar's magnetic energy reservoir. We describe a method to search for transient gravitational-wave signals associated with magnetar bursts with durations of 10 s to 1000 s of seconds. The sensitivity of this method is estimated by adding simulated waveforms to data from the sixth science run of Laser Interferometer Gravitational-wave Observatory (LIGO). We find a search sensitivity in terms of the root sum square strain amplitude of $ \newcommand{\hertz}{{\rm Hz}} \newcommand{\hrss}{h_{\rm rss}} \newcommand{\h}{\mathfrak{h}} \hrss = 1.3 \times 10^{-21}~\hertz^{-1/2}$ for a half sine-Gaussian waveform with a central frequency $f_0 = 150$ Hz and a characteristic time $\tau = 400$ s. This corresponds to a gravitational wave energy of $ \newcommand{\erg}{{\rm erg}} \newcommand{\ergs}{\erg} \newcommand{\EGW}{E_{\rm GW}} \EGW = 4.3 \times 10^{46}~{\rm \ergs}$ , the same order of magnitude as the 2004 giant flare which had an estimated electromagnetic energy of $ \newcommand{\unsim}{\mathord{\sim}} \newcommand{\erg}{{\rm erg}} \newcommand{\ergs}{\erg} \newcommand{\EEM}{E_{\rm EM}} \newcommand{\h}{\mathfrak{h}} \EEM = \unsim 1.7 \times 10^{46} (d/ 8.7~{\rm kpc}){\hspace{0pt}}^2~{\rm \ergs}$ , where d is the distance to SGR 1806-20. We present an extrapolation of these results to Advanced LIGO, estimating a sensitivity to a gravitational wave energy of $ \newcommand{\erg}{{\rm erg}} \newcommand{\ergs}{\erg} \newcommand{\EGW}{E_{\rm GW}} \newcommand{\bestUL}{4.3 \times 10^{46}} \newcommand{\bestULaLIGO}{9.0 \times 10^{44}} \newcommand{\bestULaLIGOclose}{3.2 \times 10^{43}} \EGW = \bestULaLIGOclose~{\rm \ergs}$ for a magnetar at a distance of $1.6$ kpc. These results suggest this search method can probe significantly below the energy budgets for magnetar burst emission mechanisms such as crust cracking and hydrodynamic deformation.

KW - data analysis

KW - gravitational waves

KW - magnetars

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