we propose to obtain deep photometry at 60, 90 and 160 microns of a carefully selected sample of k giants with 60 micron excess in order to determine the nature of the dust emission found in these objects. in particular we wish to investigate the possibility that the infrared excess is due to debris dust, left over from the process of planet formation, which has been re-activated as the star leaves the main sequence and evolves to the red giant phase. if this interpretation is correct, it would imply that stars can retain a cold dust shell throughout their main sequence life, and would show that the vega phenomenon may remain active throughout the life of low and intermediate mass main sequence stars. the proposed observations can only be obtained with iso, since we request observations at wavelengths and with a sensitivity that cannot be achieved with any other instrument available at present or in the near future.
Instrument
PHT03 , PHT22 , PHT40
Temporal Coverage
1996-02-17T03:40:54Z/1997-06-10T08:33:59Z
Version
1.0
Mission Description
The Infrared Space Observatory (ISO) was the worlds first true orbiting infrared observatory. Equipped with four highly-sophisticated and versatile scientific instruments, it was launched by Ariane in November 1995 and provided astronomers world-wide with a facility of unprecedented sensitivity and capabilities for a detailed exploration of the Universe at infrared wavelengths.
European Space Agency, WATERS et al., 1999, 'IR PHOTOMETRY OF K STARS WITH IR EXCESS openParPART 2closePar THE NATURE OF CIRCUMSTELLAR DUST IN K GIANTS', 1.0, European Space Agency, https://doi.org/10.5270/esa-siikke5
