In this work , we study theoretical and observational issues about pulsars ( PSRs ) , pulsar wind nebulae ( PWNe ) and supernova remnants ( SNRs ) .
In particular , the spectral modeling of young PWNe and the X-ray analysis of SNRs with magnetars comparing their characteristics with those remnants surrounding canonical pulsars .

The spectra of PWNe range from radio to \gamma -rays .
They are the largest class of identified Galactic sources in \gamma -rays increasing the number from 1 to \sim 30 during the last years .
We have developed a detailed spectral code which reproduces the electromagnetic spectrum of PWNe in free expansion ( t _ { age } \lesssim 10 kyr ) .
We shed light and try to understand issues on time evolution of the spectra , the synchrotron self-Compton dominance in the Crab Nebula , the particle dominance in PWNe detected at TeV energies and how physical parameters constrain the detectability of PWNe at TeV .
We make a systematic study of all Galactic , TeV-detected , young PWNe which allows to find correlations and trends between parameters .
We also discuss about the spectrum of those PWNe not detected at TeV and if models with low magnetized nebulae can explain the lack of detection or , on the contrary , high-magnetization models are more favorable .

Regarding the X-ray analysis of SNRs , we use X-ray spectroscopy in SNRs with magnetars to discuss about the formation mechanism of such extremely magnetized PSRs .
The alpha-dynamo mechanism proposed in the 1990 ’ s produces an energy release that should have influence in the energy of the SN explosion .
We extend the work done previously done by about the energetics of the SN explosion looking for this energy release and we look for the element ionization and the X-ray luminosity and we compare our results with other SNRs with an associated central source .