2 - Stellar Masses & Radii
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2 - Stellar Masses & Radii. Stellar Radii. “If the stars are so far away, how do we know their names?”. Stars are very far away, so how do we determine their physical sizes?. Diffraction Effects.

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Stellar Radii

“If the stars are so far away, how do we know their names?”

Stars are very far away, so how do we determine their physical sizes?


Diffraction Effects

Because light acts like a wave, it undergoes diffraction when passing through an aperture, whether it is a slit or a circular hole, etc.

A TELESCOPE OBJECTIVE ACTS LIKE A CIRCULAR APERTURE!

So the light of any star produces a diffraction pattern. THIS SETS THE MAXIMUM SPATIAL RESOLUTION THAT A TELESCOPE CAN ACHIEVE.

This is usually referred to as the Point Spread Function. In reality, other effects (aberrations) may contribute to the actual PSF of a star.

The pattern is the Fourier transform of the opening


Resolving Power

Overlap of the Point Spread Functions (PSFs)

Resolving Power (Rayleigh’s criterion)


Astronomical “Seeing”

mostly “image motion”

(“tip-tilt”)

more “image blur”


High Resolution Imaging from Space

Hubble Space Telescope - 2.4m primary mirror


Speckle Interferometry

Real-time bispectrum speckle interferometry: 76 mas resolution.

Frame rate of data recording and processing: ~ 2 frames per second.

SAO 6 m telescope, K-band.

G. Weigelt, MPI for Radioastronomy, 1999




Lunar Occultations

Grazing occultation of Aldebaran


INTERFEROMETRY

Michelson Interferometry


Keck

CHARA

VLT


IOTA JHK-spectro-interferometry

of the Mira star T Cep

wavelength range:

1.0µm (left) to 2.3µm (right)

G. Weigelt et al., 2003, SPIE 4838, 181

see: http://www.mpifr-bonn.mpg.de/div/ir-interferometry/



H- and K-band VLTI-AMBER interferograms rapid compensation

(two 1.8 m ATs; HD 48433)


Model of Altair, based on data from the Navy Prototype Optical Interferometer (Peterson et al. 2006, ApJ, 636, 1087)


Intensity (Hanbury Brown) Interferometry Optical Interferometer (Peterson et al. 2006, ApJ, 636, 1087)


Space Interferometry Mission (SIM) Optical Interferometer (Peterson et al. 2006, ApJ, 636, 1087)

Cancelled


Pipe Dream? Optical Interferometer (Peterson et al. 2006, ApJ, 636, 1087)

Terrestrial Planet Finder (TPF)


(assuming spherical stars Optical Interferometer (Peterson et al. 2006, ApJ, 636, 1087)

& uniform temperatures)

Main Sequence


How Big Are They? Optical Interferometer (Peterson et al. 2006, ApJ, 636, 1087)

http://apod.nasa.gov/apod/ap110222.html

As small as a city (neutron stars), and as large as the solar system (a few, but not really well-known)!


Stellar Masses from Binary Stars Optical Interferometer (Peterson et al. 2006, ApJ, 636, 1087)

Optical Doubles – 2 stars in the line of sight with no physical relationship.

Visual Binaries – Two physically related stars orbiting one another that can be resolved independently.

β Cyg = “Albireo”


R. Pogge Optical Interferometer (Peterson et al. 2006, ApJ, 636, 1087)

(OSU)

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Astrometric Binaries Optical Interferometer (Peterson et al. 2006, ApJ, 636, 1087)– Physically the same as a visual binary, except that one member is too faint to be detected.

Eclipsing Binaries – here, the plane of the orbit is so close to the line of sight that the stars pass in front of one another as they orbit their mutual center of mass.

Spectrum Binaries –Unresolved binary where the spectra of both stars are visible, but no orbital motion is detected through the Doppler effect.

Spectroscopic Binaries – Here, the orbital velocity and orbital inclination provide a Doppler shift large enough to be detected.

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For a pair of stars with masses Optical Interferometer (Peterson et al. 2006, ApJ, 636, 1087)m1 and m2, located a1 and a2 from the center of mass:

We don’t measure a’s directly, but the angular separation α in arcsec

Kepler’s 3rd Law:

in “astronomer’s units”:

Remember, if you can, stick with “astronomer’s units”!!


Masses from Spectroscopic Binaries Optical Interferometer (Peterson et al. 2006, ApJ, 636, 1087)

We see only the radial component of the orbital velocity

So we measure:

Similarly,

But you need to know i pretty well

In many cases you see only the spectrum of star 1 and all you can find is the mass function:


L vs M for Main Sequence Stars Optical Interferometer (Peterson et al. 2006, ApJ, 636, 1087)

The Main Sequence is a sequence of masses


How Massive Are They? Optical Interferometer (Peterson et al. 2006, ApJ, 636, 1087)

About 1/12 the Sun (brown dwarf boundary) to ~200 time the Sun


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