REVIEW 8 cited by
Gamma-ray binaries and related systems
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
Signed reviews
read the original abstract
After initial claims and a long hiatus, it is now established that several binary stars emit high (0.1-100 GeV) and very high energy (>100 GeV) gamma rays. A new class has emerged called 'gamma-ray binaries', since most of their radiated power is emitted beyond 1 MeV. Accreting X-ray binaries, novae and a colliding wind binary (eta Car) have also been detected - 'related systems' that confirm the ubiquity of particle acceleration in astrophysical sources. Do these systems have anything in common ? What drives their high-energy emission ? How do the processes involved compare to those in other sources of gamma rays: pulsars, active galactic nuclei, supernova remnants ? I review the wealth of observational and theoretical work that have followed these detections, with an emphasis on gamma-ray binaries. I present the current evidence that gamma-ray binaries are driven by rotation-powered pulsars. Binaries are laboratories giving access to different vantage points or physical conditions on a regular timescale as the components revolve on their orbit. I explain the basic ingredients that models of gamma-ray binaries use, the challenges that they currently face, and how they can bring insights into the physics of pulsars. I discuss how gamma-ray emission from microquasars provides a window into the connection between accretion--ejection and acceleration, while eta Car and novae raise new questions on the physics of these objects - or on the theory of diffusive shock acceleration. Indeed, explaining the gamma-ray emission from binaries strains our theories of high-energy astrophysical processes, by testing them on scales and in environments that were generally not foreseen, and this is how these detections are most valuable.
Forward citations
Cited by 8 Pith papers
-
Why do massive stars form bow shocks? Bulk ISM motion as the main driver of bow shock formation and geometry
Bulk interstellar gas motion, not stellar motion, dominates most massive star bow shocks; only about 21% are classical aligned bow shocks.
-
Large-scale emission from gamma-ray binaries: the case of LS 5039
The arcminute X-ray emission around LS 5039 is consistently explained as synchrotron radiation from electrons accelerated at the termination shock of the mixed stellar/pulsar wind, with different source ages giving co...
-
The IACOB project XVIII. Prevalence of short-period binaries among Galactic helium rich O-type stars
In 45 O-type binaries, all seven helium-rich systems are short-period runaways, suggesting binary interaction is the main cause of helium enrichment.
-
Fermi-LAT and FAST observation of the gamma-ray binary HESS J0632+057
Fermi-LAT data spanning 15 years yield a power-law GeV spectrum for HESS J0632+057 with a possible 10-100 GeV turnover, and FAST observations set a 2 microJy upper limit on radio pulsations from the system.
-
Combined VERITAS and NuSTAR observations of the gamma-ray binary HESS J0632+057
New NuSTAR and VERITAS spectra of HESS J0632+057 are well fitted by a pulsar-wind shock model, yielding a degenerate constraint with wind magnetization around 0.003 to 0.03 at the shock.
-
Searching for links between energetic millisecond pulsars and repeating fast radio bursts
Wideband observations show M28A giant pulses differ from FRB 20200120E bursts in duration, luminosity, timing statistics, and spectral structure, yielding no strong evidence for a direct link.
-
SKAO and Gamma-Ray Synergies
Overview of synergies between SKA radio observations and gamma-ray facilities for studying transient, variable, and steady GeV-TeV sources.
-
X-Ray Views of Galactic Accreting Pulsars in High-Mass X-Ray Binaries
A concise review of the timing, spectral, and polarization properties of accreting X-ray pulsars in high-mass X-ray binaries, including recent IXPE results.
Discussion (0). Continue with ORCID to comment.