Rotating radio transient

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A rotating radio transient ( German  rapidly rotating volatile radio source ) is a pulsar , a rotating neutron star having a directional synchrotron radiation along its magnetic dipole axis, wherein a search for individual pulses than in a better Fourier analysis can be found. The interval between individual detectable pulses is between 10 and 10,000 seconds with a rotation period of the RRATs between 0.1 and seven seconds.

properties

The rotating radio transient were first described as transient radio bursts in 2005. This was the result of a targeted search for individual bursts in the area of radio radiation , instead of searching for pulsars with the help of precisely repeating signals, as was previously the case. The width of the individual radio pulses is between two and 30 milliseconds. The RRAT show period jumps like normal pulsars. In the radio range, the pulses are heavily modulated when switched on, but without any indication of a modulation frequency. The relative lengthening of the period of rotation is greater in RRAT than in normal pulsars; this is attributed to a stronger magnetic field and correspondingly low age.

In the X-ray range , thermal radiation could be detected by at least one RRAT; the derived temperature of more than a million Kelvin confirms nature as a neutron star. The point source is surrounded by an extensive halo in the X-ray range, which is caused by a pulsar wind nebula or by scattering. At least two regular pulsars were temporarily perceived as rotating radio transients .

Difference to pulsars

The hypothesis most frequently cited is that RRATs are just an extreme form of nulling and giant pulses in normal pulsars. Given the current numbers of known rotating radio transients, this assumption leads to an increase in the rate of formation of neutron stars by a factor of five to six. This means that the number of core collapse supernovae in the Milky Way was underestimated by a corresponding factor or that other development channels lead to the formation of pulsars.

Alternatively, changes in the number of free charge carriers or in the current density of the magnetosphere could cause the pulses to cease, or the radiation would be blocked by a recurrence of matter ejected from a supernova .

The presumption that the Fast Radio Bursts are extragalactic  RRAT is now considered discarded. The luminosity of the Fast Radio Bursts is many orders of magnitude higher than that of the Rotating Radio Transients, and FRBs do not seem to repeat themselves - with one exception - either.

Examples

Individual evidence

  1. ^ EF Keane and MA McLaughlin: Rotating Radio Transients . In: Astrophysics. Solar and Stellar Astrophysics . 2012, arxiv : 1109.6896 .
  2. ^ MA McLaughlin et al .: Transient radio bursts from rotating neutron stars . In: Astrophysics. Solar and Stellar Astrophysics . 2005, arxiv : astro-ph / 0511587v2 .
  3. ↑ B.-Y. Cui, J. Boyles, MA McLaughlin, N. Palliyaguru: Timing Solution and Single-pulse Properties for Eight Rotating Radio Transients . In: Astrophysics. Solar and Stellar Astrophysics . 2017, arxiv : 1706.08412v1 .
  4. ↑ BM Gaensler et al .: Chandra Smells a RRAT: X-ray detection of a rotating radio transient . In: Astrophysics. Solar and Stellar Astrophysics . 2006, arxiv : astro-ph / 0608311 .
  5. ↑ A. Camero-Arranz et al .: The extended X-ray emission around RRATJ1819-1458 . In: Astrophysics. Solar and Stellar Astrophysics . 2012, arxiv : 1211.7340 .
  6. ↑ A. Esamdin, D. Abdurixit, RN Manchester, HB Niu: PSR B0826-34: Sometimes a RRAT . In: Astrophysics. Solar and Stellar Astrophysics . 2012, arxiv : astro-ph / 0608311 .
  7. ↑ S. Burke Spolaor: Rotating Radio Transients and Their Place Among pulsar . In: Astrophysics. Solar and Stellar Astrophysics . 2012, arxiv : 1212.1716 .
  8. ↑ Alice K. Harding: The Neutron Star Zoo . In: Astrophysics. Solar and Stellar Astrophysics . 2012, arxiv : 1302.0869v1 .
  9. ^ G. Taylor et al .: Observations of Rotating Radio Transients with the First Station of the Long Wavelength Array . In: Astrophysics. Solar and Stellar Astrophysics . 2016, arxiv : 1610.04270v1 .
  10. ↑ EF Keane: Classifying RRATs and FRBs . In: Astrophysics. Solar and Stellar Astrophysics . 2015, arxiv : 1512.02513v1 .