scholarly journals Publisher’s Note: Upper limits on gravitational wave emission from 78 radio pulsars [Phys. Rev. D76, 042001 (2007)]

2008 ◽  
Vol 77 (6) ◽  
Author(s):  
B. Abbott ◽  
R. Abbott ◽  
R. Adhikari ◽  
J. Agresti ◽  
P. Ajith ◽  
...  
Keyword(s):  
Gravitational Wave ◽  
Radio Pulsars ◽  
Upper Limits ◽  
Wave Emission

scholarly journals Upper limits on gravitational wave emission from 78 radio pulsars

2007 ◽  
Vol 76 (4) ◽  
Author(s):  
B. Abbott ◽  
R. Abbott ◽  
R. Adhikari ◽  
J. Agresti ◽  
P. Ajith ◽  
...  
Keyword(s):  
Gravitational Wave ◽  
Radio Pulsars ◽  
Upper Limits ◽  
Wave Emission

Gravitational wave emission from galactic radio pulsars

1997 ◽  
Vol 56 (2) ◽  
pp. 859-863 ◽  
Author(s):  
J. A. de Freitas Pacheco ◽  
J. E. Horvath
Keyword(s):  
Gravitational Wave ◽  
Radio Pulsars ◽  
Wave Emission ◽  
Galactic Radio

scholarly journals Constraints from LIGO O3 Data on Gravitational-wave Emission Due to R-modes in the Glitching Pulsar PSR J0537–6910

2021 ◽  
Vol 922 (1) ◽  
pp. 71
Author(s):  
R. Abbott ◽  
T. D. Abbott ◽  
S. Abraham ◽  
F. Acernese ◽  
K. Ackley ◽  
...  
Keyword(s):  
Energy Conservation ◽  
Gravitational Wave ◽  
Gravitational Waves ◽  
Theoretical Models ◽  
X Ray ◽  
Spin Evolution ◽  
Upper Limits ◽  
Wave Emission ◽  
Using Data

Abstract We present a search for continuous gravitational-wave emission due to r-modes in the pulsar PSR J0537–6910 using data from the LIGO–Virgo Collaboration observing run O3. PSR J0537–6910 is a young energetic X-ray pulsar and is the most frequent glitcher known. The inter-glitch braking index of the pulsar suggests that gravitational-wave emission due to r-mode oscillations may play an important role in the spin evolution of this pulsar. Theoretical models confirm this possibility and predict emission at a level that can be probed by ground-based detectors. In order to explore this scenario, we search for r-mode emission in the epochs between glitches by using a contemporaneous timing ephemeris obtained from NICER data. We do not detect any signals in the theoretically expected band of 86–97 Hz, and report upper limits on the amplitude of the gravitational waves. Our results improve on previous amplitude upper limits from r-modes in J0537-6910 by a factor of up to 3 and place stringent constraints on theoretical models for r-mode-driven spin-down in PSR J0537–6910, especially for higher frequencies at which our results reach below the spin-down limit defined by energy conservation.

Upper Limits on Gravitational-Wave Emission in Association with the 27 Dec 2004 Giant Flare of SGR1806-20

2005 ◽  
Vol 95 (8) ◽  
Author(s):  
L. Baggio ◽  
M. Bignotto ◽  
M. Bonaldi ◽  
M. Cerdonio ◽  
L. Conti ◽  
...  
Keyword(s):  
Gravitational Wave ◽  
Upper Limits ◽  
Wave Emission ◽  
Giant Flare

scholarly journals ENERGETICS OF THE SUPERFLARE FROM SGR1806-20 AND A POSSIBLE ASSOCIATED GRAVITATIONAL WAVE BURST

2005 ◽  
Vol 20 (36) ◽  
pp. 2799-2804 ◽  
Author(s):  
J. E. HORVATH
Keyword(s):  
Gravitational Wave ◽  
Energy Release ◽  
Gamma Rays ◽  
Gamma Ray ◽  
Expected Frequency ◽  
Upper Limits ◽  
Wave Emission ◽  
Soft Gamma Repeater ◽  
First Time

We discuss in this paper the energetics of large gamma-ray superflares observed from Soft-Gamma Repeater sources. The last recorded event has in fact ruled out some models for the energy release. For the first time actual information about a possible associated gravitational wave emission may have been gathered from the LIGO data, even in the case that most of the energy was emitted in gamma-rays. Even upper limits on the amplitude of the latter h at the expected frequency fc≤2 kHz may be useful to further constrain the remaining mechanisms.

scholarly journals Gravitational waves from mountains in newly born millisecond magnetars

2021 ◽  
Vol 502 (4) ◽  
pp. 4680-4688
Author(s):  
Ankan Sur ◽  
Brynmor Haskell
Keyword(s):  
Gravitational Wave ◽  
Gravitational Waves ◽  
Massive Star ◽  
Gamma Ray ◽  
Dipole Radiation ◽  
X Ray ◽  
Binary Neutron Star ◽  
Spin Period ◽  
Lower Maximum ◽  
Wave Emission

ABSTRACT In this paper, we study the spin-evolution and gravitational-wave luminosity of a newly born millisecond magnetar, formed either after the collapse of a massive star or after the merger of two neutron stars. In both cases, we consider the effect of fallback accretion; and consider the evolution of the system due to the different torques acting on the star, namely the spin-up torque due to accretion and spin-down torques due to magnetic dipole radiation, neutrino emission, and gravitational-wave emission linked to the formation of a ‘mountain’ on the accretion poles. Initially, the spin period is mostly affected by the dipole radiation, but at later times, accretion spin the star up rapidly. We find that a magnetar formed after the collapse of a massive star can accrete up to 1 M⊙, and survive on the order of 50 s before collapsing to a black hole. The gravitational-wave strain, for an object located at 1 Mpc, is hc ∼ 10−23 at kHz frequencies, making this a potential target for next-generation ground-based detectors. A magnetar formed after a binary neutron star merger, on the other hand, accretes at the most 0.2 M⊙ and emits gravitational waves with a lower maximum strain of the order of hc ∼ 10−24, but also survives for much longer times, and may possibly be associated with the X-ray plateau observed in the light curve of a number of short gamma-ray burst.

scholarly journals Interpreting the X-ray afterglows of gamma-ray bursts with radiative losses and millisecond magnetars

2020 ◽  
Vol 499 (4) ◽  
pp. 5986-5992
Author(s):  
Nikhil Sarin ◽  
Paul D Lasky ◽  
Gregory Ashton
Keyword(s):  
Gravitational Wave ◽  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
Dipole Radiation ◽  
X Ray ◽  
Radiative Efficiency ◽  
Central Engine ◽  
Radiative Losses ◽  
Wave Emission ◽  
Prompt Emission

ABSTRACT The spin-down energy of millisecond magnetars has been invoked to explain X-ray afterglow observations of a significant fraction of short and long gamma-ray bursts. Here, we extend models previously introduced in the literature, incorporating radiative losses with the spin-down of a magnetar central engine through an arbitrary braking index. Combining this with a model for the tail of the prompt emission, we show that our model can better explain the data than millisecond-magnetar models without radiative losses or those that invoke spin-down solely through vacuum dipole radiation. We find that our model predicts a subset of X-ray flares seen in some gamma-ray bursts. We can further explain the diversity of X-ray plateaus by altering the radiative efficiency and measure the braking index of newly born millisecond magnetars. We measure the braking index of GRB061121 as $n=4.85^{+0.11}_{-0.15}$ suggesting the millisecond-magnetar born in this gamma-ray burst spins down predominantly through gravitational-wave emission.

scholarly journals Searching for gravitational-wave bursts from cosmic string cusps with the Parkes Pulsar Timing Array

2020 ◽  
Vol 501 (1) ◽  
pp. 701-712
Author(s):  
N Yonemaru ◽  
S Kuroyanagi ◽  
G Hobbs ◽  
K Takahashi ◽  
X-J Zhu ◽  
...  
Keyword(s):  
False Alarm ◽  
Gravitational Wave ◽  
Cosmic String ◽  
Cosmic Strings ◽  
False Alarm Probability ◽  
String Tension ◽  
Detection Algorithm ◽  
Pulsar Timing ◽  
Upper Limits ◽  
Pulsar Timing Array

ABSTRACT Cosmic strings are potential gravitational-wave (GW) sources that can be probed by pulsar timing arrays (PTAs). In this work we develop a detection algorithm for a GW burst from a cusp on a cosmic string, and apply it to Parkes PTA data. We find four events with a false alarm probability less than 1 per cent. However further investigation shows that all of these are likely to be spurious. As there are no convincing detections we place upper limits on the GW amplitude for different event durations. From these bounds we place limits on the cosmic string tension of Gμ ∼ 10−5, and highlight that this bound is independent from those obtained using other techniques. We discuss the physical implications of our results and the prospect of probing cosmic strings in the era of Square Kilometre Array.

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