scholarly journals Influence of the dispersion relation on the Unruh effect according to the relativistic Doppler shift method

2021 ◽  
Vol 103 (8) ◽  
Author(s):  
F. Hammad ◽  
A. Landry ◽  
D. Dijamco
Keyword(s):  
Dispersion Relation ◽  
Doppler Shift ◽  
Unruh Effect ◽  
Shift Method

scholarly journals Photon velocity, power spectrum in Unruh effect with modified dispersion relation

2020 ◽  
Vol 129 (3) ◽  
pp. 30002
Author(s):  
Arnab Mukherjee ◽  
Sunandan Gangopadhyay ◽  
Manjari Dutta
Keyword(s):  
Dispersion Relation ◽  
Power Spectrum ◽  
Unruh Effect ◽  
Modified Dispersion Relation

Determination of the alignment of a 7Li beam by means of the Doppler-shift method

1981 ◽  
Vol 179 (3) ◽  
pp. 541-543 ◽  
Author(s):  
Z. Moroz ◽  
R. Böttger ◽  
P. Egelhof ◽  
K.-H. Möbius ◽  
G. Tungate ◽  
...  
Keyword(s):  
Doppler Shift ◽  
Shift Method

scholarly journals specphot: a comparison of spectroscopic and photometric exoplanet follow-up methods

2020 ◽  
Vol 495 (1) ◽  
pp. 734-742 ◽  
Author(s):  
Benjamin F Cooke ◽  
Don Pollacco
Keyword(s):  
Radial Velocity ◽  
Doppler Shift ◽  
Planetary System ◽  
Signal To Noise Ratio ◽  
High Accuracy ◽  
Signal To Noise ◽  
Shift Method ◽  
System Parameters ◽  
Transit Method

ABSTRACT We set out a simulation to explore the follow-up of exoplanet candidates. We look at comparing photometric (transit method) and spectroscopic (Doppler shift method) techniques using three instruments: Next-Generation Transit Survey, High-Accuracy Radial-velocity Planetary Search, and CORALIE. We take into account the precision of follow-up and required observing time in attempt to rank each method for a given set of planetary system parameters. The methods are assessed on two criteria: signal-to-noise ratio (S/N) of the detection and follow-up time before characterization. We find that different follow-up techniques are preferred for different regions of parameter space. For S/N, we find that the ratio of spectroscopic to photometric S/N for a given system goes like $R_{\rm p}/P^{{1}/{3}}$. For follow-up time, we find that photometry is favoured for the shortest period systems (<10 d) as well as systems with small planet radii. Spectroscopy is then preferred for systems with larger radius, and thus more massive planets (given our assumed mass–radius relationship). Finally, we attempt to account for the availability of telescopes and weight the two methods accordingly.

Sign in / Sign up

Export Citation Format

Share Document