Handbook of Pulsar Astronomy

By D. R. Lorimer, Michael Kramer. 2004

529 citations recorded by the source corpus.

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Citations in the corpus

• A real-time fast radio burst: polarization detection and multiwavelength follow-up (2014, methodology): “…rotation is quantified by the rotation measure, RM ∝ ∫ d 0 neB‖dl , (3) where d is the distance to the source, ne is the electron column density, and B‖ is the magnetic field parallel to the line of sight such that the rotation angle of the linear polarization ∆Ψ = RMλ2 (Lorimer & Kramer 2004).”
• Pulsar searches and timing with the square kilometre array (2009, background): “Lorimer & Kramer 2005 ) in the study of the Milky Way, globular clusters, the evolution and collapse of massive stars, the formation and evolution of binary systems, the properties of super-dense matter, extreme plasma physics, tests of theories of gravity, the detection of gravitational waves, and ”
• The astrophysics of nanohertz gravitational waves (2018, background): “The time delay between the Earth and barycentric reference frames is given by (Lorimer and Kramer 2012):”
• FRBCAT: The Fast Radio Burst Catalogue (2016, methodology): “The DM index for the propagation of waves through a cold plasma is α = 2 (Lorimer & Kramer 2004).”
• Possible periodic activity in the repeating FRB 121102 (2020, methodology): “Then, we computed the fluence for each pulse using the radiometer equation (Lorimer & Kramer 2004).”
• EIGHT γ-RAY PULSARS DISCOVERED IN BLIND FREQUENCY SEARCHES OF FERMI LAT DATA (2010, methodology): “…in Table 5.274 To compute the minimum pulsar flux that could have been detected in these observations, we use the modified radiometer equation (e.g. Lorimer & Kramer 2004): Smin = β (S/N)minTsys G √ nptint∆f √ W P −W (3) where β is the instrument-dependent factor due to digitization and other…”
• On the formation history of Galactic double neutron stars (2018, background): “The formation rate and log Bayes factor of model (04) are R = 30.95 per Milky Way equivalent galaxy per Myr and logK = −2.50.”
• THE SECOND FERMI LARGE AREA TELESCOPE CATALOG OF GAMMA-RAY PULSARS (2013, background): “7.10 on page 174 of Lorimer & Kramer 2004) assuming a minimum signal-to-noise ratio of 5 for a detection and a pulse duty cycle of 10%.”
• Upper Bounds on the Low-Frequency Stochastic Gravitational Wave Background from Pulsar Timing Observations: Current Limits and Future Prospects (2006, background): “Pulsar timing observations (see Lorimer & Kramer 2005, Edwards, Hobbs & Manchester 2006 for a review of the techniques) provide a unique opportunity to study low-frequency (10−9 − 10−7 Hz) gravitational waves (GWs) (e.g., Sazhin 1978, Detweiler 1979, Bertotti,”
• Progenitors of gravitational wave mergers: binary evolution with the stellar grid-based code ComBinE (2018, background): “In extreme cases, a merger (and thus a sGRB) may occur less than 1 Myr after the formation of a double NS system, see figure 40 in Tauris et al. (2017).”
• PULSAR J0453+1559: A DOUBLE NEUTRON STAR SYSTEM WITH A LARGE MASS ASYMMETRY (2015, methodology): “To estimate the upper limit on the companion’s pulsed mean flux density in our line of sight, S ,max we used the radiometer equation (Lorimer & Kramer 2004), using the parameters of the search observations and accounting for dispersive smearing at the DM of the system and a minimum S/N of 10.”