Comparar métodos
Examine os métodos selecionados lado a lado; as linhas que diferem ficam destacadas.
| Array de Tempo de Pulsares× | Epoch of Reionization 21-cm× | |
|---|---|---|
| Área | Astronomia | Astronomia |
| Família | Process / pipeline | Process / pipeline |
| Ano de origem≠ | 1979 | 1990 |
| Autor original≠ | Stephen Detweiler | David Scott |
| Tipo≠ | Observational timing method | Radio observational method |
| Fonte seminal≠ | Sazhin, M. V. (1978). Opportunities for detecting ultralong gravitational waves. Soviet Astronomy, 22, 36-38. link ↗ | Scott, D., & Rees, M. J. (1990). The 21-cm signature of the ionization of the intergalactic medium. Monthly Notices of the Royal Astronomical Society, 247, 510-516. link ↗ |
| Outros nomes | PTA, Millisecond Pulsar Timing, Pulsar Timing Residuals | EoR 21-cm, Hydrogen Line Observations, 21-cm Signal Mapping |
| Relacionados | 3 | 3 |
| Resumo≠ | A pulsar timing array uses multiple millisecond pulsars as a distributed network of gravitational wave detectors across the galaxy. Proposed theoretically by Stephen Detweiler in 1979, this method exploits the extraordinary timing precision of pulsars to detect the subtle spacetime distortions caused by gravitational waves. In 2023, the first evidence for a stochastic background of gravitational waves was announced using pulsar timing arrays. | The 21-centimeter line observation of neutral hydrogen is a powerful technique for studying the Epoch of Reionization, when the first stars and galaxies ionized the intergalactic medium about 13 billion years ago. Proposed by Scott and Rees in 1990, this method probes the universe's transition from the dark ages to the cosmic dawn through the characteristic hyperfine line emission of hydrogen. |
| ScholarGateConjunto de dados ↗ |
|
|