Libri ricevuti e recensioni

Bertotti, B.; Careri, G.; Quaranta, A. Alberigi; Ascoli, A.; Reggiani, L.; Degiorgio, V.

doi:10.1007/bf02899960

Cited by 2 publications

(4 citation statements)

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“…(13). 5 We also take advantage of the useful fact that p(i) = Ti T1 dt/P (t), and the expressions above can be derived by noting that ∆P , ∆T i andṖ are small quantities. Henceforth, to avoid clutter, we suppress the i, j indices and use bold-faced symbols to represent matrices or vectors, wherever no confusion would arise.…”

Section: Discussionmentioning

confidence: 99%

“…It 4 In most of the paper, we simply use P to denote the unperturbed period, when there is no danger of confusion. 5 We have implicitly assumed that the periastron time shift from external GWs is entirely due to their effect on the orbital period. In reality, there can be an (apparent) periastron time shift coming from center-of-mass linear momentum imparted by GWs, or from fluctuations in the orbital eccentricity.…”

Section: Discussionmentioning

confidence: 99%

“…Versions of this idea have been discussed in pioneering work by [1][2][3][4][5][6]. The subject lay dormant for many years, perhaps due in part to the focus shifting to PTAs in discussions of pulsars as a detection tool.…”

Section: Introductionmentioning

confidence: 99%

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Binary systems as resonance detectors for gravitational waves

2013

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Gravitational waves at suitable frequencies can resonantly interact with a binary system, inducing changes to its orbit. A stochastic gravitational-wave background causes the orbital elements of the binary to execute a classic random walk, with the variance of orbital elements growing with time.The lack of such a random walk in binaries that have been monitored with high precision over long time-scales can thus be used to place an upper bound on the gravitational-wave background. Using periastron time data from the Hulse-Taylor binary pulsar spanning ∼ 30 years, we obtain a bound of hc < 7.9 × 10 −14 at ∼ 10 −4 Hz, where hc is the strain amplitude per logarithmic frequency interval. Our constraint complements those from pulsar timing arrays, which probe much lower frequencies, and ground-based gravitational-wave observations, which probe much higher frequencies. Interesting sources in our frequency band, which overlaps the lower sensitive frequencies of proposed spacebased observatories, include white-dwarf/supermassive black-hole binaries in the early/late stages of inspiral, and TeV scale preheating or phase transitions. The bound improves as (time span) −2 and (sampling rate) −1/2 . The Hulse-Taylor constraint can be improved to ∼ 3.8 × 10 −15 with a suitable observational campaign over the next decade. Our approach can also be applied to other binaries, including (with suitable care) the Earth-Moon system, to obtain constraints at different frequencies. The observation of additional binary pulsars with the SKA could reach a sensitivity of hc ∼ 3 × 10 −17 .

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Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

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Binary systems as resonance detectors for gravitational waves

2013

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“…Alternatively, it is not necessary for the pulsar to rotate very fast if the pulsar is a solid quark star (Xu 2003;Zhou et al 2004), because a solid quark star could have a larger elastic deformation, max ∼ 10 −4 (Owen 2005). Suppose there is no other dissipation mechanism other than gravitational wave radiation, then the typical damping time-scale of precession is τ rigid θ = 1.8×10 6 yr( /10 −7 ) −2 (P/0.001 s) 4 (I/10 45 g cm 2 ) −1 ∼ 10 6 -10 12 yr (Bertotti & Anile 1973;Cutler & Jones 2001). Therefore the bursting activity should remain with approximately the same period and duration provided that it is a solid quark star.…”

Section: T H E P U L S a Rmentioning

confidence: 99%

GCRT J1745—3009: a precessing radio pulsar?

Zhu

2006

Monthly Notices of the Royal Astronomical Society: Letters

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A unique transient bursting radio source, GCRT J1745−3009, has been discovered near the direction of the Galactic Centre. The explanation of this phenomenon is still an open question, although some efforts to understand its nature have been made. This Letter shows that most of the observed features can be reproduced by our proposed precessing pulsar model. It is found that the precession angle of the pulsar should be larger (≳15°) than that of previously known precessing pulsars, which have a precession angle ≲10°, if the beam width of the pulsar is larger than 10°. The pulsar could be a nulling (or even extremely nulling) radio pulsars to account for the transient nature of the source. This model can be confirmed if a pulsar is detected at the position of the source. The pulsar could hardly be a normal neutron star (but could probably be a solid quark star) if the spin period of the pulsar is detected to be ≳10 ms in the future.

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Libri ricevuti e recensioni

Cited by 2 publications

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Binary systems as resonance detectors for gravitational waves

Binary systems as resonance detectors for gravitational waves

GCRT J1745—3009: a precessing radio pulsar?

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