1 / 13

Exploring Stars: Radii Measurement Methods and Temperature Determination

Learn about measuring star radii through direct methods like interferometry, occultations, and eclipsing binaries, and determining temperatures using bolometric flux and model photospheres.

zoey
Télécharger la présentation

Exploring Stars: Radii Measurement Methods and Temperature Determination

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Measuring Radii and Temperatures of Stars • Definitions (again…) • Direct measurement of radii • Speckle • Interferometry • Occultations • Eclipsing binaries • Photometric determinations of radii • Bolometric flux • Surface brightness • Absolute flux • Determining temperatures • Absolute flux • Model photospheres • Colors • Balmer jump • Hydrogen lines • Metal lines R = radius r = distance R/r=angular diameter

  2. Stellar Diameters • Angular diameters typically measured in milli-arcseconds (mas) • Angular diameter (in radians) given by physical diameter divided by distance The diameter of Aldebaran is ~40 RSUN. Its distance is about 19 pc. The angular diameter of Aldebaran is … (work in cgs or MKS units or work in AU and use the definition of a parsec) What would the angular diameter of the Sun be at 10 pc?

  3. Speckle Diameters • The diffraction limit of 4-m class telescopes is ~0.02” at 4000A, comparable to the diameter of some stars • The seeing disk of a large telescope is made up of the rapid combination of multiple, diffraction-limited images • 2-d Fourier transform of short exposures will recover the intrinsic image diameter • Only a few stars have large enough angular diameters. • Speckle mostly used for binary separations

  4. Interferometry • 7.3-m interferometer originally developed by Michelson • Measured diameters for only 7 K & M giants • Until recently, only a few dozen stars had interferometric diameters

  5. CHARA Interferometer on Mt. Wilson

  6. CHARA Delay Compensator

  7. Other Methods • Occultations • Moon used as knife-edge • Diffraction pattern recorded as flux vs. time • Precision ~ 0.5 mas • A few hundred determined • Eclipsing binaries • Photometry gives ratio of radii to semi-major axes • Velocities give semi-major axes (i=90)

  8. Photometric Methods – Bolometric Flux • Must know bolometric flux of star • Distance • Temperature • Bolometric correction • Calibrated with • Stellar models • Nearby stars with direct measurements

  9. Surface Brightness • To avoid uncertainties in Teff and BC • Determine PV as a function of B-V PV(B-V)=logTeff – 0.1BC • PV(B-V) is known as the “surface brightness function” • Calibrate with directly measured diameters

  10. Absolute Flux • Determine the apparent monochromatic flux at some wavelength, Fn • From a model that fits the spectral energy distribution, compute the flux at the star’s surface, Fn • From the ratio of Fn/Fn, compute the radius • The infrared flux method is just this method applied in the infrared.

  11. Hipparcos! • The European Hipparcos satellite determined milli-arcsec parallaxes for more than 100,000 stars. • Distances are no longer the major source of uncertainty in radius determinations for many stars • Zillions of stars within range of the Keck interferometer (3 mas at 2m) • USNO & CHARA interferometers < 1 mas • Surface structure • Pulsations • Circumstellar material

More Related