Children and Young People in Domestic Violence Shelters

Chanmugam, Amy

doi:10.1007/978-981-287-035-3_5

Cited by 4 publications

(2 citation statements)

References 42 publications

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“…The pulsar ages calculated from spin-down luminosity, however, are generally not reliable measures of real age, because energy loss-rates are not expected to be constant due to likely variations in magnetic field strength (e.g. see Chanmugam et al 1995) and cases of inconsistency between SNR age and pulsar spin-down age are well-known (e.g. Gotthelf: & Halpern 2009).…”

Section: 4mentioning

confidence: 99%

A Supernova Remnant Counterpart for HESS J1832−085

Maxted¹,

Filipović²,

Hurley‐Walker³

et al. 2019

ApJ

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We examine the new Galactic supernova remnant (SNR) candidate, G23.11+0.18, as seen by the Murchison Widefield Array (MWA) radio telescope. We describe the morphology of the candidate and find a spectral index of −0.63±0.05 in the 70-170 MHz domain. A coincident TeV gamma-ray detection in High-Energy Stereoscopic System (HESS) data supports the SNR nature of G23.11+0.18 and suggests that G23.11+0.18 is accelerating particles beyond TeV energies, thus making this object a promising new cosmic ray hadron source candidate. The remnant cannot be seen in current optical, infrared and X-ray data-sets. We do find, however, a dip in CO-traced molecular gas at a line-of-sight velocity of ∼85 km s −1 , suggesting the existence of a G23.11+0.18 progenitor wind-blown bubble. Furthermore, the discovery of molecular gas clumps at a neighbouring velocity towards HESS J1832−085 adheres to the notion that a hadronic gamma-ray production mechanism is plausible towards the north of the remnant. Based on these morphological arguments, we propose an interstellar medium association for G23.11+0.18 at a kinematic distance of 4.6±0.8 kpc.

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Section: 4mentioning

confidence: 99%

A Supernova Remnant Counterpart for HESS J1832−085

Maxted¹,

Filipović²,

Hurley‐Walker³

et al. 2019

ApJ

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“…The spindown of pulsars due to the intense magnetic fields that surround them is a phenomenon that will significantly impact on the younger pulsars which can lose a large amount of rotational energy due to physical processes such as electromagnetic and gravitational multipole radiation. The evolution of pulsars has been studied in great detail [4][5][6][7][8][9][10][11][12][13][14][15][16][17][18][19][20][21].The first observations of gravitational waves by Advanced LIGO are identified as black hole mergers, namely GW150914 [22], GW151226 [23] and a less significant candidate LVT151012 [24]. Recently, GWs from another such merger, GW170104 has been reported [25].…”

mentioning

confidence: 99%

An analytic approach for the study of pulsar spindown

Chishtie¹,

Zhang²,

Valluri³

2018

Class. Quantum Grav.

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In this work we develop an analytic approach to study pulsar spindown. We use the monopolar spindown model by , which assumes an inverse linear law of magnetic field decay of the pulsar, to extract an all-order formula for the spindown parameters which are expressed in terms of modified Bessel functions. We further extend the analytic model to incorporate the quadrupole term that accounts for the emission of gravitational radiation, and obtain expressions for the period P and frequency f in terms of transcendental equations. We derive the period of the pulsar evolution as an approximate first order solution in the small parameter present in the full solution. We find that the first three spindown parameters of the Crab, PSR B1509-58, PSR B0540-69 and Vela pulsars are within their known bounds providing a consistency check on our approach. After the four detections of gravitational waves from binary black hole coalescence and a binary neutron merger 170814, which was a novel joint gravitational and electromagnetic detection, a detection of gravitational waves from pulsars will be the next landmark in the field of multi-messenger gravitational wave astronomy.introduced to ensure that the braking indices defined in terms of the frequency and higher derivatives are in agreement with the trajectories in the P ¬Ṗ diagram for pulsar evolution, where P andṖ denote the pulsar period and its time derivative. Their detailed analysis of the stationary multipole model ruled out the possibility of a time independent evolutionary equation for the pulsar frequency. Their time dependent multipole model included dynamics of the pulsar magnetic moment and thereby the decay of the magnetic field, B(t). They show in their analysis that an inverse linear decay proposed by Chanmugham and Sang [3], in contrast to an exponential decay law for pulsar magnetic field [4], did a better fit of the evolutionary trajectories of the four pulsars studied namely the Crab, PSR B1509-58, PSR B0540-69 and Vela. Following their approach, we use an inverse linear decay law for B(t). The spindown of pulsars due to the intense magnetic fields that surround them is a phenomenon that will significantly impact on the younger pulsars which can lose a large amount of rotational energy due to physical processes such as electromagnetic and gravitational multipole radiation. The evolution of pulsars has been studied in great detail [4][5][6][7][8][9][10][11][12][13][14][15][16][17][18][19][20][21].The first observations of gravitational waves by Advanced LIGO are identified as black hole mergers, namely GW150914 [22], GW151226 [23] and a less significant candidate LVT151012 [24]. Recently, GWs from another such merger, GW170104 has been reported [25]. GW170814 was coherently observed by the advanced Virgo and two advanced LIGO detectors, produced by the coalescence of two stellar mass black holes. Recently, a neutron merger has been detected by both GW and electromagnetic observations [26]. With increasing detector sensitivity of LIGO, VIRGO and the upcoming KAG...

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