Gamma-ray bursts / Andrew Levan.

Περιλαμβάνει βιβλιογραφικές παραπομπές.

1. A historical primer -- 1.1. A lesson in serendipity -- 1.2. GRB phenomenology -- 1.3. The early years -- 1.4. Suggested models for GRB creation -- 1.5. Intensive efforts and large samples -- 1.6. The fireball shock model -- 1.7. The long-GRB afterglow revolution -- 1.8. Redshifts and host galaxies -- 1.9. The supernova connection -- 1.10. GRB energetics -- 1.11. The Neil Gehrels Swift era -- 1.12. New insights from fermi -- 1.13. Multimessenger astronomy -- 1.14. Summary

2. Prompt emission -- 2.1. Observational properties -- 2.2. Origin of the prompt emission -- 2.3. Summary

3. Afterglow emission -- 3.1. The first afterglow searches -- 3.2. X-ray afterglows -- 3.3. Optical afterglows -- 3.4. Radio/submillimeter afterglows -- 3.5. Emission processes -- 3.6. Evidence for relativistic beaming

4. Central engines -- 4.1. The requirement of a central engine -- 4.2. Black hole central engines -- 4.3. Magnetar central engines -- 4.4. Central engines in other astrophysical transients -- 4.5. Summary

5. Long-GRB progenitors -- 5.1. The GRB-supernova connection -- 5.2. Observational constraints on stellar masses and sizes -- 5.3. Other populations of long-duration GRBs -- 5.4. Low-luminosity GRBs -- 5.5. Extremely long gamma-ray transients -- 5.6. Constraints for GRB production -- 5.7. Binary or single?

6. Short-GRB progenitors -- 6.1. Introduction -- 6.2. Progenitor models -- 6.3. Prompt emission properties -- 6.4. Afterglow properties -- 6.5. Host galaxy properties -- 6.6. Locations -- 6.7. Redshifts and energetics -- 6.8. Radioactively driven transients -- 6.9. Gravitational-wave emission

7. GRBs as cosmological probes -- 7.1. A range of cosmological probes -- 7.2. Science from high-z GRB afterglows -- 7.3. GRBs beyond z [tilde operator] 5 -- 7.4. GRBs from population iii stars -- 7.5. The universal star formation rate -- 7.6. Cosmological parameters from GRBs -- 7.7. The GRB hubble diagram

8. Long-GRB host galaxies -- 8.1. Early observations -- 8.2. GRB hosts in the galaxy zoo -- 8.3. Basic properties of long-GRB hosts -- 8.4. Building meaningful samples of GRB hosts -- 8.5. GRBs hosts at optical and ir wavelengths -- 8.6. GRB hosts at submillimeter and radio wavelengths -- 8.7. GRB hosts as tools to probe progenitors -- 8.8. GRB hosts as tools to probe distant galaxies -- 8.9. Burst locations and environments -- 8.10. Comparative properties of GRB hosts with other core-collapse events

9. Multimessenger astronomy -- 9.1. From multiwavelength to multimessenger astronomy -- 9.2. Gravitational waves -- 9.3. Sources of gravitational-wave emission -- 9.4. Gravitational-wave horizons -- 9.5. Prospect for joint detections -- 9.6. Electromagnetic searches in black hole-black hole mergers -- 9.7. GW 170817 and GRB 170817a -- 9.8. Gravitational wave-electromagnetic detections : questions for the future -- 9.9. Neutrino emission -- 9.10. Ultra-high-energy cosmic rays -- 9.11. Summary

10. GRB astronomy : summary and future outlook -- 10.1. Challenges for the future -- 10.2. Possibilities for future GRB detection missions -- 10.3. The crucial role of follow-up -- 10.4. Summary.

As the most powerful explosion that occurs in the universe, gamma-ray bursts (GRBs) are one of the most exciting topics being studied in astrophysics. Creating more energy than the Sun does in its entire lifetime, GRBs create a blaze of light that will outshine every other object visible in the sky, enabling us to measure galaxies that are several million years old.