Diego F. Torres' research

How does the multifrequency spectral energy distribution of pulsar wind nebulae evolve with time, and how is this evolution coupled to their dynamics? How can we model the additional complexity introduced by diffusion, particle escape, anisotropies, pulsar kicks, and age while keeping the calculations computationally tractable?

What is the impact of reverberation, and how strongly does it depend on the surrounding environment? How can it be modelled in practice to interpret middle-aged and evolved nebulae?

How many pulsar wind nebulae exist in the Galaxy, and how many are observable, or expected to become observable, at different wavelengths?

How can confused nebulae be distinguished from isolated ones in forthcoming observational data? How can nebular classification be accelerated to enable population studies on practical timescales?

Do magnetars host nebulae? If so, are magnetar nebulae physically distinct from ordinary pulsar wind nebulae, and how are they affected by magnetar flares?

What makes a pulsar bright at different frequencies, and how can we predict which pulsars are likely to be detectable across the electromagnetic spectrum?

What population properties can be extracted from the systematic modelling of large samples of gamma-ray pulsars?

What relevant information is stored in pulsar light curves?  How unique is it? How similar are light curves from different pulsars? What makes them alike?

Can the observed spectral energy distribution be used directly as a predictor of the intrinsic properties of a pulsar?

Are magnetars physically distinct from the rest of the pulsar population, or do they represent an extreme part of the same broader family?

How do magnetar flares affect the nebulae surrounding them?

What are the physical connections among magnetars, fast radio bursts, and gamma-ray binaries?

How and when does accretion lead to gamma-ray emission?

To what extent can magnetospheric pulsations be maintained during accretion?

What drives transitional pulsar behavior?

What is the physical mechanism behind transitional pulsar states and modes?

Are pulsars active during the low modes of the accretion state? How quickly do magnetospheres reconstruct themselves if they are disrupted by episodic accretion?

Are magnetospheres restored to the same configuration after a mode change?

What fraction of pulsars in compact binaries actually undergo such transitions?

Are all gamma-ray binaries pulsar-powered systems? Why, how, and when do they emit at high energies?

Do pulsars and their nebulae make a significant contribution to cosmic rays?

What is the impact of cosmic rays in the vicinity of their acceleration sites?

How far can helium and other nuclei travel before losing their identity or coherence?

How are star-forming regions, across different spatial scales, connected to cosmic-ray production and propagation?

What are the composition and origin of ultra-high-energy cosmic rays?