Sentences with phrase «eclipsing binary»

Firstly, he is interested in the study of stellar interiors from the observational point of view by means of eclipsing binary stars.

The photom... ▽ More Wide - field searches for transiting extra-solar giant planets face the difficult challenge of separating true transit events from the numerous false positives caused by isolated or blended eclipsing binary systems.

He is also interested in eclipsing binaries in Local Group galaxies that can serve as distance indicators.

Our spectra show no evidence of line bisector variations that would indicate a blended eclipsing binary star.

Most notable is the noise - weighted robust averaging of multi-quarter photo - center offsets derived from difference image analysis which identifies likely background eclipsing binaries.

When eclipsing binaries orbit each other closely, within about 10 days or less, Fleming and co-authors wondered, do tides — the gravitational forces each exerts on the other — have «dynamical consequences» to the star system?

While current datasets at Vanderbilt are being used to search for eclipsing binaries and extrasolar planets, this system can be easily reconfigured for a wide variety of data sources.

When eclipsing binaries orbit each other closely, within about 10 days or less, the study authors wondered, do tides — the gravitational forces each exerts on the other — have «dynamical consequences» to the star system?

David Fleming, a doctoral student at the University of Washington, and colleagues study eclipsing binaries, or those where the orbital plane is so near the line of sight, both stars are seen to cross in front of each other.

This search is contaminated by a large fraction of false positives, caused by different eclipsing binary configurations that might be confused with a transiting planet.

In addition, we identify 16 targets as likely eclipsing binaries, based on their light curve morphology.

Help scientists solve the mystery of epsilon Aurigae, a mysterious, bright, eclipsing binary variable star that has baffled scientists since 1821

For candidates with transit depths in the range from 0.1 - 0.4 %, CoRoT detections are nearly complete, and this difference from predictions is probably real and dominated by a lower than expected abundance of diluted eclipsing binaries.

Results from these tests provide also in many cases insights into the nature of the sources of the false positives, which are generally produced by one of several kinds of configurations involving eclipsing binaries (EB).

A well - known eclipsing binary makes up part of Algol, a multiple - star system in the constellation Perseus.

Eclipsing Binary Science Via the Merging of Transit and Doppler Exoplanet Survey Data - A Case Study With the MARVELS Pilot Project and SuperWASP

For low - mass eclipsing binary stars, the method of eclipse minimum timing allows astronomers to search for smaller masses than those feasible with radial velocity measurements.

Unlike eclipsing binaries, the other two types of variable stars are intrinsically variable — that is to say, their own output of radiant energy fluctuates with time.

Recent experience has highlighted the need for careful analysis to eliminate astronomical systems where light from a faint eclipsing binary is blended with that from a bright star.

A blend may consist of a background or foreground eclipsing binary (or star - planet pair) whose eclipses are attenuated by the light of the candidate and possibly other stars within the photometric aperture.

Abstract: Wide - field searches for transiting extra-solar giant planets face the difficult challenge of separating true transit events from the numerous false positives caused by isolated or blended eclipsing binary systems.

We are in the process of identi - fying and measuring parameters for detached eclipsing binaries (dEBs) in the open clusters in the Kepler and CoRoT fields.

In a paper accepted for publication in Astrophysical Journal, lead author David Fleming, a UW astronomy doctoral student, studies eclipsing binaries, or those where the orbital plane is so near the line of sight, both stars are seen to cross in front of each other.

Astronomers are searching for variable stars in NGC 206, particularly pulsating stars known as Cepheids and eclipsing binary star systems.

Next they ruled out a false positive, usually caused by an eclipsing binary - star system in the background, with two relatively small telescopes on the ground, which offer better spatial resolution than COROT does.

The two bodies are aligned to form an eclipsing binary, with the red star periodically passing in front of the blue, blocking it from our view.

The reason is simple statistics: It's extremely unlikely to encounter two background eclipsing binaries (or one background binary and one genuine planet) at the same location.

But other observations need to confirm the true planetary nature of these candidate events, because the observed dips may also be due to an eclipsing binary star in the background whose light blends with the foreground star studied by Kepler.

In the original work by Brown, slightly different classes of false positives were used: MPU (main - sequence star with a giant planet); MSU (undiluted binaries); and the two types of diluted binaries, MSDF (an eclipsing binary + a third non-related star) and MSDT (triple systems).

Light curve of Algol (Beta Persei), an eclipsing variable, or eclipsing binary, star system.

Specifically, eclipsing binary stars can be used to study the stellar mass - radius relationship and to test predictions of theoretical stellar evolution models.

In an eclipsing binary, the two stars pass in front of each other in turn, creating eclipses and periodic dimming of their combined light.

By cross-referencing 24 binary stars found in the MARVELS Pilot Project with SuperWASP photometry, we find two new eclipsing binaries, TYC 0272 -00458-1 and TYC 1422 -01328-1, which we use as case studies to develop a general approach to eclipsing binaries in survey data.

CM Draconis Aa has a close, double - lined spectroscopic companion Ab, with which it forms a non-contact, eclipsing binary, and a wide common - proper - motion companion B. Stars Aab and B have an observed separation of about 420 AUs (25.7»).

Some are geometric variables, as in the eclipsing binaries considered earlier.

Piper Michelle Reid, Dripping Springs High School, Dripping Springs, Texas Photometric and Spectroscopic Analysis for the Determination of Physical Parameters of an Eclipsing Binary Star System

In 1967, the reddish component was found to be an eclipsing binary by Olin Jeuck Eggen and Allan Sandage.

We obtained follow - up optical spectra of 105/141 candidate host stars and 8/16 eclipsing binaries to improve stellar properties and to identify spectroscopic binaries.

Here, we predict the properties of the transiting planets that TESS will detect along with the eclipsing binary stars that produce false - positive photometric signals.

We obtained follow - up optical spectra of 105/141 candidate host stars and 8/16 eclipsing binaries to improve stellar properties and to identify spectroscop... ▽ More We present 151 planet candidates orbiting 141 stars from K2 campaigns 5 - 8 (C5 - C8), identified through a systematic search of K2 photometry.

This goal requires knowledge of the incidence of false positives such as eclipsing binaries in the background of the targets, or physically bound to them, which can mimic the photometric signal of a transiting planet.

In order to detect as many of these false positives as possible, we perform ephemeris matching among all transiting planet, eclipsing binary, and variable star sources.