Mauna Loa Solar Observatory
| Mauna Loa Solar Observatory | |
|---|---|
|
MLSO domes on Mauna Loa | |
| Organization | National Center for Atmospheric Research |
| Location | Mauna Loa, Hawaii |
| Coordinates | 19°32′10″N 155°34′34″W / 19.536°N 155.576°WCoordinates: 19°32′10″N 155°34′34″W / 19.536°N 155.576°W |
| Altitude | 3,394 meters (11,135 ft) |
| Established | 1965 |
| Website | Mauna Loa Solar Observatory |
Mauna Loa Solar Observatory (MLSO) is a solar observatory located on the slopes of Mauna Loa on the island of Hawaii in the U.S. state of Hawaii. It is operated by the High Altitude Observatory (HAO), a laboratory within the National Center for Atmospheric Research (NCAR). The MLSO sits on property managed by the Mauna Loa Observatory (MLO), which is part of the U.S. Department of Commerce National Oceanic and Atmospheric Administration (NOAA). MLSO was built in 1965.[1]
The MLSO is tasked with monitoring the solar atmosphere and recording data on plasmic and energetic emissions from the chromosphere and corona. Studies of coronal mass ejections (CMEs) are also conducted at MLSO. A number of non-solar astronomical observatories are located at the site. The MLSO instruments record images of the solar disk and limb every 3 minutes for 3–10 hours daily starting at 17:00 UT, weather permitting.
Instruments
Current instruments
- The Coronal Multi-channel Polarimeter (CoMP) monitors the magnetic field in the corona by recording the strength and polarization of light received from corona.[2]
- The Precision Solar Photometric Telescope (PSPT) produces highly accurate images of the photosphere at five different wavelengths.[3]
Former instruments
- The Advanced Coronal Observing System (ACOS) is a set of instruments for monitoring the chromosphere on a shared mount.[3]
- The Coronado Solarmax 60 (CS60) is a small refractor built by Meade Instruments which provides H-alpha disk and limb images.[3]
- Chromospheric Helium-I Imaging Photometer (CHIP) observes at a wavelength which is an emission line for non-ionized helium (He I) in order to monitor the chromosphere.[3]
- The Polarimeter for Inner Coronal Studies (PICS) produced H-alpha disk and limb digital images from 1994 to 1997. It was replaced by the CS60.[3]
- The Digital Prominence Monitor (DPM) produced H-alpha disk and limb digital images from 1994 to 1997. It was replaced by the PICS.[3]
- The Prominence Monitor (PMON) produced H-alpha disk and limb images on film from 1980 to 1994. It was replaced by the DPM.[3]
- The Mark-III K-Coronameter (Mk3) operated from 1980 to 1998, and was replaced by the MK4.[3]
Non-MLSO instruments
- The Array for Microwave Background Anisotropy (AMiBA) is a radio telescope array designed to observe the cosmic microwave background and the Sunyaev-Zel'dovich effect. It consists of seven 0.58 m (23 in) receivers on a hexapod mount.[4]
- The Global Oscillations Network Group (GONG) has deployed an observing station to study helioseismology.[5]
- The Variable Young Stellar Object Survey (VYSOS) is a project to monitor young stars and star-forming regions. It consists of a 13.5 cm (5.3 in) refractor and a 50 cm (20 in) reflector in separate domes.[6]
See also
References
- ↑ "Mauna Loa Solar Observatory (HAO/NCAR): slideshow". Mauna Loa Solar Observatory. Retrieved 2012-01-15.
- ↑ "COSMO Site - The Coronal Multi-channel Polarimeter". High Altitude Observatory. Retrieved 2012-01-15.
- ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 3.7 "Mauna Loa Solar Observatory (HAO/NCAR): About MLSO and Its Instrumentation". Mauna Loa Solar Observatory. Retrieved 2012-01-15.
- ↑ "AMIBA - Introduction". Academica Sinica Institute of Astronomy and Astrophysics. Retrieved 2012-01-15.
- ↑ "NSO/GONG: Site - Mauna Loa". National Solar Observatory. Retrieved 2012-01-15.
- ↑ "VYSOS Variable Young Stellar Object Survey". University of Hawaii Institute for Astronomy. Retrieved 2012-01-15.