Carbon atmosphere discovered on neutron star
Scientists determined that the neutron star in Cassiopeia A has an ultra-thin coating of carbon.
Provided by the Chandra X-ray Center, Cambridge, Massachusetts
November 4, 2009
Evidence for a thin veil of carbon has been found on the neutron star in the Cassiopeia A supernova remnant. This discovery made with NASA's Chandra X-ray Observatory resolves a 10-year mystery surrounding this object.
"The compact star at the center of this famous supernova remnant has been an enigma since its discovery," said Wynn Ho of the University of Southampton. "Now we finally understand that it can be produced by a hot neutron star with a carbon atmosphere."
By analyzing Chandra's X-ray spectrum — like a fingerprint of energy — and applying it to theoretical models, Ho and Craig Heinke, from the University of Alberta, determined that the neutron star in Cassiopeia A (Cas A) has an ultra-thin coating of carbon. This is the first time scientists have confirmed the composition of an atmosphere of an isolated neutron star.
The Chandra "First Light" image of Cas A in 1999 revealed a previously undetected point-like source of X-rays at the center. This object was presumed to be a neutron star — the typical remnant of an exploded star — but researchers were unable to understand its properties. Defying astronomers' expectations, this object did not show any X-ray or radio pulsations or any signs of radio pulsar activity.
By applying a model of a neutron star with a carbon atmosphere to this object, Ho and Heinke found that the region emitting X-rays would uniformly cover a typical neutron star. This would explain the lack of X-ray pulsations because — like a light bulb that shines consistently in all directions — this neutron star would be unlikely to display any changes in its intensity as it rotates.
Scientists previously have used a neutron star model with a hydrogen atmosphere giving a much smaller emission area, corresponding to a hot spot on a typical neutron star, which should produce X-ray pulsations as it rotates. Interpreting the hydrogen atmosphere model without pulsations would require a tiny size, consistent only with exotic stars made of strange quark matter.
"Our carbon veil solves one of the big questions about the neutron star in Cas A," said Heinke. "People have been willing to consider some weird explanations, so it's a relief to discover a less peculiar solution."
Unlike most astronomical objects, neutron stars are small enough to understand on a human scale. For example, neutron stars typically have a diameter of only about 14 miles [23 kilometers]. The atmosphere of a neutron star is on an even smaller scale. The researchers calculate that the carbon atmosphere is only about 4 inches [10 centimeters] thick because it has been compressed by a surface gravity that is 100 billion times stronger than on Earth.
"For people who are used to hearing about immense sizes of things in space, it might be a surprise that we can study something so small," said Ho. "It's also funny to think that such a thin veil over this star played a key role in frustrating researchers."
In Earth's time frame, the estimated age of the neutron star in Cas A is only several hundred years, making it about 10 times younger than other neutron stars with detected surface emission. Therefore, the Cas A neutron star gives a unique window into the early life of a cooling neutron star.
The carbon itself comes from a combination of material that has fallen back after the supernova and nuclear reactions on the hot surface of the neutron star, which convert hydrogen and helium into carbon.
The X-ray spectrum and lack of pulsar activity suggest that the magnetic field on the surface of this neutron star is relatively weak. Similarly low magnetic fields are implied for several other young neutron stars by study of their weak X-ray pulsations. Scientists don't know whether these neutron stars will have low magnetic fields for their entire lives and never become radio pulsars, or whether processes in their interior will lead to the development of stronger magnetic fields as they age.