Eclipsing Pulsar Promises Clues to Crushed Matter
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ECLIPSING PULSAR PROMISES CLUES TO CRUSHED MATTER
Astronomers using NASA's Rossi X-ray Timing Explorer (RXTE) have found
the first fast X-ray pulsar to be eclipsed by its companion star.
Further studies of this unique stellar system will shed light on some
of the most compressed matter in the universe and test a key
prediction of Einstein's relativity theory.
The pulsar is a rapidly spinning neutron star -- the crushed core of a
massive star that long ago exploded as a supernova. Neutron stars pack
more than the Sun's mass into a ball nearly 60,000 times smaller. With
estimated sizes between 10 and 15 miles across, a neutron star would
just span Manhattan or the District of Columbia.
"It's difficult to establish precise masses for neutron stars,
especially toward the higher end of the mass range theory predicts,"
said Craig Markwardt at NASA's Goddard Space Flight Center in
Greenbelt. "As a result, we don't know their internal structure or
sizes as well as we'd like. This system takes us a step closer to
narrowing that down."
Known as Swift J1749.4-2807 -- J1749 for short -- the system erupted
with an X-ray outburst on April 10. During the event, RXTE observed
three eclipses, detected X-ray pulses that identified the neutron star
as a pulsar, and even recorded pulse variations that indicated the
neutron star's orbital motion.
J1749 was discovered in June 2006, when a smaller eruption brought it
to the attention of NASA's Swift satellite. Observations by Swift,
RXTE and other spacecraft revealed that the source was a binary system
located 22,000 light-years away in the constellation Sagittarius and
that the neutron star was actively capturing, or accreting, gas from
its stellar partner. This gas gathers into a disk around the neutron
star.
"Like many accreting binary systems, J1749 undergoes outbursts when
instabilities in the accretion disk allow some of the gas to crash
onto the neutron star," said Tod Strohmayer, RXTE's project scientist
at Goddard.
The pulsar's powerful magnetic field directs infalling gas onto the
star's magnetic poles. This means that the energy release occurs in
hot spots that rotate with the neutron star, producing fast X-ray
pulses. How fast? J1749 is spinning 518 times a second -- a city-sized
sphere rotating as fast as the blades of a kitchen blender.
In addition, the pulsar's orbital motion imparts small but regular
changes in the frequency of the X-ray pulses. These changes indicate
that the stars revolve around each other every 8.8 hours.
During the week-long outburst, RXTE observed three periods when
J1749's X-ray emission briefly disappeared. Each eclipse, which lasts
36 minutes, occurs whenever the neutron star passes behind the normal
star in the system.
"This is the first time we've detected X-ray eclipses from a fast
pulsar that is also accreting gas," Markwardt said. "Using this
information, we now know the size and mass of the companion star with
unprecedented accuracy."
By comparing RXTE observations across the theoretical mass range for
neutron stars, the astronomers determined that J1749's normal star
weighs in with about 70 percent of the Sun's mass -- but the eclipses
indicate that the star is 20 percent larger than it should be for its
mass and apparent age.
"We believe that the star's surface is 'puffed up' by radiation from
the pulsar, which is only about a million miles away from it,"
Markwardt explained. "This additional heating probably also makes the
star's surface especially disturbed and stormy."
Writing about their findings in the July 10 issue of The Astrophysical
Journal Letters, Markwardt and Strohmaye
one orbital variable needed to nail down the mass of the pulsar, which
is estimated to be between about 1.4 and 2.2 times the Sun's mass.
"We need to detect the normal star in the system with optical or
infrared telescopes," Strohmayer said. "Then we can measure its motion
and extract the same information about the pulsar that the pulsar's
motion told us about the star."
However, a pioneering X-ray measurement well within the capability of
RXTE may make a hunt for the star irrelevant.
One consequence of relativity is that a signal -- such as a radio wave
or an X-ray pulse -- experiences a slight timing delay when it passes
very close to a massive object. First proposed by Irwin Shapiro at the
Massachusetts Institute of Technology (MIT) in Cambridge, Mass., in
1964 as a new test for predictions of Einstein's relativity, the delay
has been demonstrated repeatedly using radio signals bounced off of
Mercury and Venus and experiments involving spacecraft communications.
"High-precision measurements of the X-ray pulses just before and after
an eclipse would give us a detailed picture of the entire system,"
Strohmayer said. For J1749, the predicted Shapiro delay is 21
microseconds, or 10,000 times faster than the blink of an eye. But
RXTE's superior timing resolution allows it to record changes 7 times
faster.
With only three eclipses observed during the 2010 outburst, RXTE
didn't capture enough data to reveal a large delay. However, the
measurements set a limit on how massive the normal star can be. The
study shows that if the star's mass was greater than 2.2 times the
Sun's, RXTE would have seen the delay.
"We believe this is the first time anyone has set realistic limits for
this effect at X-ray wavelengths outside of our solar system,"
Markwardt noted. "The next time J1749 has an outburst, RXTE absolutely
could measure its Shapiro delay."
Launched in late 1995, RXTE is second only to Hubble as the longest
serving of NASA's currently operating astrophysics missions. RXTE
-- in 1998 and continues to provide a unique observing window into the
extreme environments of neutron stars and black holes.
Image:
http://www.nasa.gov/topics/universe/features/eclipsing-pulsar.html
Caption:
J1749 is the first accreting millisecond pulsar to undergo eclipses.
The pulsar and its companion star are separated by 1.22 million miles,
or about five times the distance between Earth and the Moon.
Irradiated by the pulsar's intense X-rays, the star's outer layers
puff up to make it about 20 percent larger than a star of its mass and
age should be. This image includes additional data about the system.
Credit:
NASA/GSFC