What about the Double Pulsar?
The “Double Pulsar” Binary (DPB) is a binary system containing 2 pulsars, named “A” and “B”.
The Double Pulsar is formally known as: J0737-3039A/B.
It’s properties include:
- “A” has a spin period of 22.7 milliseconds
- “B” has a spin period of 2.77 seconds (100 times slower than “A”)
- “A” has a mass of 1.33 M-Sun
- “B” has a mass of 1.25 M-Sun
- The orbital period of “A” and “B” around each other is 2.45 hours (shortest known)
So, the question is: How does the NS-Capture Theory explain the existence of the Double Pulsar Binary?
It seems unlikely, if not impossible, for 2 neutron stars in space to collide and capture each other, so this origin is ruled out immediately (there would be no tidal interaction between the NSs, although the magnetic fields would interact to some degree).
The way the Double Pulsar binary must have formed is the following.
- A giant star captured neutron star A, and as time went by evolved into an O-type super-giant, where pulsar A became deeply embedded in the super-giant atmosphere, and spun up to a rapid rotation period, somewhere in the vicinity of its current value of 22.7 ms.
- The super-giant, now containing neutron star A, then captured neutron star B, which became a close binary around the super-giant, and spun up to a period close to its current period of 2.77 sec.
- The system could then be viewed as a central star with 2 planets: an inner planet “A”, and an outer planet “B”.
- Similar to other O-type super-giants, the central star became so hot that it became gravitationally unbound, and exploded in a supernova.
- Left behind were the two pulsars “A” and “B” that ended up orbiting each other in the form they are observed today.
That’s it! Presto! A ready-made Double Pulsar Binary.
1/13/19: Update on double binary pulsar:
The double pulsar has been in the news fairly frequently, primarily with consideration as to likelihood that it might prove to be a steady measurable source of gravity waves.
However, the concern of this web site at this time is primarily focused on the proof of the NS-Capture theory.
As described above, NS-Capture suggests the DPB (double pulsar binary) most likely formed by a 2nd NS colliding with a SuperGiant that already contained a NS companion in some intermediate stage of spin-up before the inevitable SNE.
However, even with the suggestion of the 2nd collision, there is probably still a population problem, given the lifetime of SuperGiant X-ray Binaries (SGXB’s) being on the order of one million years or less. How could a population of DPB’s be maintained if the collision rate of a NS is significantly less than the 1 million year SGXB lifetime?
The answer lies in the relative lifetime of the DPB vs a SGXB. i.e. even though the collision rate of a NS with an existing SGXB may be significantly less than 1 per million years, if the DB has a life expectancy significantly greater than 1 million years, then the collision rate could be much less than one per million years.
In addition, if the supposition is correct that all SG’s contain an embedded NS pulsar, then all SG’s are potential targets to create a DPB.
Why would the DPB have a longer lifetime? Most likely there is ongoing spin orbit interaction with the two FP’s in the DPB, where orbital energy is absorbed by the FP’s causing their spin rate to be maintained much longer than an ordinary spinning down isolated FP. In particular, since the orbit can become extremely small before the FP’s have any chance of direct collision (whatever that may entail), it seems likely that the spin-orbit interaction is capable of keeping both members of the DPB in the FP state for many times the lifetime of a SGXB.
Note: the real capture rate would be the NS’s against ALL the SGXB’s that would exist in the lifetime of a DB. Therefore, the population issue of double collision between NS’s and SGXB’s appears to have a perfectly logical solution within the context of the NS-Capture theory.
