Top: 100 single pulses from the 253-ms pulsar B0950+08, demonstrating pulse-to-pulse variability in shape and intensity. Bottom: Cumulative profile for this pulsar over 5 minutes (about 1200 pulses); this approaches the reproducible standard profile. Observations taken with the Green Bank Telescope [58]. (Stairs, unpublished.)
Pulse profile shapes for PSR J1740–3052 at multiple frequencies, aligned by pulse timing. The full pulse period is displayed at each frequency. The growth of an exponential scattering tail at low frequencies is evident. All observations taken with the Green Bank Telescope [58] (Stairs, unpublished), except for the 660-MHz profile which was acquired at the Parkes telescope [107, 121].
Pulse profile of the fastest rotating pulsar, PSR B1937+21, observed with the 76-m Lovell telescope at Jodrell Bank Observatory [69]. The top panel shows the total-intensity profile derived from a filterbank observation (see text); the true profile shape is convolved with the response of the channel filters. The lower panel shows the full-Stokes observation with a coherent dedispersion instrument [123, 122]. Total intensity is indicated by black lines, and linear and circular power by red and blue lines, respectively. The position angle of the linear polarization is plotted twice. The coherent dedispersion observation results in a much sharper and more detailed pulse profile, less contaminated by instrumental effects and more closely resembling the pulse emitted by the rotating neutron star. Much better timing precision can be obtained with these sharper pulses.
“Polarization” of a nearly circular binary orbit under the influence of a forcing vector
, showing the relation between the forced eccentricity 
, the eccentricity evolving under the
general-relativistic advance of periastron 
, and the angle 
. (After [145].)
Measured neutron star masses as a function of age. The solid lines show predicted changes in the average neutron star mass corresponding to hypothetical variations in
, where 
implies 
. (From [135], used by permission.)
The parabola indicates the predicted accumulated shift in the time of periastron for PSR B1913+16, caused by the decay of the orbit. The measured values of the epoch of periastron are indicated by the data points. (From [144], courtesy Joel Weisberg.)
Mass–mass diagram for the PSR B1913+16 system, using the
and
parameters listed in Table 2. The uncertainties are smaller than the widths of the lines. The
lines intersect at the point given by the masses derived under the DDGR formalism. (From [144],
courtesy Joel Weisberg.)
Mass–mass diagram for the PSR B1534+12 system. Labeled curves illustrate 68% confidence ranges of the DD parameters listed in Table 3. The filled circle indicates the component masses according to the DDGR solution. The kinematic correction for assumed distance d = 0.7 ± 0.2 kpc has been subtracted from the observed value of
; the uncertainty
on this kinematic correction dominates the uncertainty of this curve. A slightly larger distance
removes the small apparent discrepancy between the observed and predicted values of this parameter.
(After [125].)
Portions of the tensor-biscalar
plane permitted by timing observations of
PSRs B1913+16, B1534+12, and B1855+09 up to
1992. Values lying above the curve labeled “a” are incompatible with the measured 
and
parameters for PSR B1913+16. The curves labeled “b” and “d” give the
allowed ranges of 
and 
for PSRs B1913+16 and B1534+12,
respectively, fitting for the two neutron-star masses as well as 
and 
, using data available
up to 1992. The vertical lines labeled “c” represent limits on 
from the SEP-violation test using
PSR B1855+09 [43]. The dot at (0,0) corresponds to GR. (Reprinted by permission
from Nature [133], Ⓒ 1992, Macmillan Publishers Ltd.)
The parameter space in the non-linear
, 
gravitational theory, for neutron stars
described by a polytrope equation of state. The regions below the various curves are allowed by various
pulsar timing limits, by solar-system tests (“1PN”), and by projected LIGO/VIRGO observations of
NS–NS and NS–BH inspiral events. The shaded region is allowed by all tests. The plane and limits
are symmetric about 
. (From [40]; used by permission.)
Solid line: predicted value of the Shapiro delay in PSR J0437–4715 as a function of orbital phase, based on the observed inclination angle of 42° ± 9°. For such low-eccentricity binaries, much of the Shapiro delay can be absorbed into the orbital Roemer delay; what remains is the
periodicity shown. The points represent the timing residuals for the
pulsar, binned in orbital phase, and in clear agreement with the shape predicted from the inclination
angle. (Reprinted by permission from Nature [139], Ⓒ 2001, Macmillan Publishers Ltd.)
Changes in the observed pulse profile of PSR B1913+16 throughout the 1980s, due to a changing line-of-sight cut through the emission region of the pulsar. (Taken from [132]; used by permission.)
Top: change in peak separation of the relativistic double-neutron-star binary PSR B1913+16, as observed with the Arecibo (solid points, [141]) and Effelsberg (open circles, [81]) telescopes. Bottom: projected disappearance of PSR B1913+16 in approximately 2025. (Taken from [81]; used by permission.)
Hourglass-shaped beam for PSR B1913+16 derived from the symmetric-component analysis of [143]. (Taken from [143]; used by permission.)
Alternate proposed beam shape for PSR B1913+16, consisting of a symmetric cone plus an offset core. The red lines indicate an example cut through the emission region, as well as the predicted pulse peak ratio and separation as functions of time. (After [82], courtesy Michael Kramer.)
Evolution of the low-level emission surrounding the main pulse of PSR B1534+12, over a period of nearly 10 years, as measured with the Arecibo telescope [6]. (Stairs et al., unpublished.)