Optimal wavelength interval for extra-solar planet detection

2021 ◽  
Author(s):  
Marija Strojnik
Keyword(s):  
Wavelength Interval ◽  
Planet Detection ◽  
Optimal Wavelength

scholarly journals Stellar noise and planet detection. I. Oscillations, granulation and sun-like spots

2010 ◽  
Vol 6 (S276) ◽  
pp. 527-529
Author(s):  
Xavier Dumusque ◽  
Nuno C. Santos ◽  
Stéphane Udry ◽  
Cristophe Lovis ◽  
Xavier Bonfils
Keyword(s):  
Radial Velocity ◽  
Time Scales ◽  
High Precision ◽  
Habitable Zone ◽  
Planet Detection ◽  
Solar Type ◽  
Physical Phenomena ◽  
Instrumental Precision ◽  
Observational Strategy ◽  
Different Time Scales

AbstractSpectrographs like HARPS can now reach a sub-ms−1 precision in radial-velocity (RV) (Pepe & Lovis 2008). At this level of accuracy, we start to be confronted with stellar noise produced by 3 different physical phenomena: oscillations, granulation phenomena (granulation, meso- and super-granulation) and activity. On solar type stars, these 3 types of perturbation can induce ms−1 RV variation, but on different time scales: 3 to 15 minutes for oscillations, 15 minutes to 1.5 days for granulation phenomena and 10 to 50 days for activity. The high precision observational strategy used on HARPS, 1 measure per night of 15 minutes, on 10 consecutive days each month, is optimized, due to a long exposure time, to average out the noise coming from oscillations (Dumusque et al. 2011a) but not to reduce the noise coming from granulation and activity (Dumusque et al. 2011a and Dumusque et al. 2011b). The smallest planets found with this strategy (Mayor et al. 2009) seems to be at the limit of the actual observational strategy and not at the limit of the instrumental precision. To be able to find Earth mass planets in the habitable zone of solar-type stars (200 days for a K0 dwarf), new observational strategies, averaging out simultaneously all type of stellar noise, are required.

Bounds on optimal wavelength assignment with and without wavelength changers

1998 ◽  
Author(s):  
M. K. Rajesh ◽  
Kumar N. Sivarajan ◽  
Ananth Selvarajan
Keyword(s):  
Wavelength Assignment ◽  
Optimal Wavelength

Space-based planet detection using two MEMS DMs and a shaped pupil

2012 ◽  
Author(s):  
N. Jeremy Kasdin ◽  
T. Groff ◽  
A. Carlotti ◽  
R. Vanderbei
Keyword(s):  
Planet Detection

The Linear Relationship between Concentrations and UV Absorbance of Nitrobenzene

2014 ◽  
Vol 955-959 ◽  
pp. 1376-1379 ◽  
Author(s):  
Dan Wu ◽  
Kai Xiao Zhang
Keyword(s):  
Linear Relationship ◽  
Correlation Coefficient ◽  
Absorption Peak ◽  
Maximum Absorption ◽  
Uv Absorbance ◽  
Wavelength Interval ◽  
Vis Spectroscopy

This paper researched the linear relationship between UV absorbance and concentrations of nitrobenzene. It used the UV-1700 UV/VIS spectroscopy to get the absorbance diagram and analyze it. Then it calculated the absorbance of maximum absorption peak and the absorbance integration in a wavelength interval. There is a linear relationship between absorbance and concentration, the correlation coefficient is 0.981 of the maximum absorption peaks and the concentrations, and the largest correlation coefficient between concentrations and the integration of absorbance is 0.995 with the wavelength interval of 235-245 nm, which is between the two absorption peaks of 210 nm and 270 nm. Therefore, it’s a good way to use integration of absorbance in the middle of two absorption peaks to measure the concentration of nitrobenzene, which is more accurate and reliable.

Planet Detection

2012 ◽  
Author(s):  
JON JENKINS ◽  
JEFFREY SMITH ◽  
PETER TENENBAUM ◽  
JOSEPH TWICKEN ◽  
JEFFREY CLEVE
Keyword(s):  
Planet Detection

scholarly journals Using the Sun to estimate Earth-like planet detection capabilities

2015 ◽  
Vol 583 ◽  
pp. A118 ◽  
Author(s):  
N. Meunier ◽  
A.-M. Lagrange ◽  
S. Borgniet ◽  
M. Rieutord
Keyword(s):  
The Sun ◽  
Planet Detection ◽  
Detection Capabilities

scholarly journals Microorganism adhesion experimental study using silicon dioxide

2018 ◽  
Author(s):  
Roberts Lozins ◽  
Dzintars Ozoliņš
Keyword(s):  
Silicon Dioxide ◽  
Near Infrared ◽  
Gram Negative Bacteria ◽  
Wavelength Interval ◽  
Absorption Properties ◽  
Gram Positive ◽  
Gram Negative ◽  
Suitable Material ◽  
Absorption Of Light ◽  
Physical Absorption

AbstractIn this study, yeast, Gram positive and Gram negative bacteria were attached to silicon dioxide microparticles or silica in order to measure their absorbance, also known as physical absorption of light, changes using spectrophotometry. The goal of the study was to determine if spectrophotometry is an effective way to distinguish microorganisms and if microorganisms have an affinity for silicon dioxide since it is a suitable material for the production of prostheses. The experiment was done by examining the light absorption properties of yeast, Gram positive and Gram negative bacteria in a spectrophotometer with and without silicon dioxide microparticles. During the experiment there have been several promising results. First of all, the spectrophotometers presented graphs of yeast were noticeably different from the graphs of both Gram positive and Gram negative bacteria. Secondly, the absorption of light in both Gram positive and Gram negative bacteria at near infrared (700-1500 nm) wavelengths increased when silicon dioxide microparticles were added to the suspension, unlike yeast. When silicon dioxide microparticles were added to yeast, the absorption of light decreased during the whole wavelength interval of the spectrophotometer measurement. The results indicate that spectrophotometry could be used to distinguish yeast from bacteria and possibly bacteria from each other. The results also suggest that silicon dioxide should not be used in the production of prostheses since it could be a favourable material for the development of biofilms.

Sign in / Sign up

Export Citation Format

Share Document