This shows you the differences between two versions of the page.
Both sides previous revision Previous revision Next revision | Previous revision | ||
usic:chara_array_chara [2019/07/10 18:44] gail_stargazer |
usic:chara_array_chara [2019/07/10 18:51] gail_stargazer |
||
---|---|---|---|
Line 5: | Line 5: | ||
====== Center for High Angular Resolution Astronomy (CHARA) ====== | ====== Center for High Angular Resolution Astronomy (CHARA) ====== | ||
- | [[http:// | + | [[http:// |
* Gravity darkening and oblateness of rapidly rotating main sequence stars. | * Gravity darkening and oblateness of rapidly rotating main sequence stars. | ||
Line 15: | Line 15: | ||
* Images of interacting binaries. | * Images of interacting binaries. | ||
* Images of a binary star system in eclipse. | * Images of a binary star system in eclipse. | ||
- | * Precision masses | + | * Precision |
* Direct detection of high contrast companions around Cepheids, RS CVn, and Be stars. | * Direct detection of high contrast companions around Cepheids, RS CVn, and Be stars. | ||
* Structure and physical properties of circumstellar disks around Be stars. | * Structure and physical properties of circumstellar disks around Be stars. | ||
* Images of disks and winds around young stellar objects. | * Images of disks and winds around young stellar objects. | ||
- | * Earliest | + | * Early measurements of the angular expansion of a nova after an eruption. |
* Direct images of starspots. | * Direct images of starspots. | ||
* Images of convection cells on supergiant stars. | * Images of convection cells on supergiant stars. | ||
Line 25: | Line 25: | ||
===== Overview of the CHARA Array ===== | ===== Overview of the CHARA Array ===== | ||
- | \\ Georgia State University’s Center for High Angular Resolution Astronomy (CHARA) operates an optical/ | + | \\ Georgia State University’s Center for High Angular Resolution Astronomy (CHARA) operates an optical/ |
+ | |||
+ | The Beam Combining Laboratory (BCL) contains six beam combiners with complementary regimes of wavelength, sensitivity, measurement precision, and number of telescopes combined. The Array control system is capable of running | ||