  Elements with low First Ionization Potential (FIP) are known to be three to
four times more abundant in active region loops of the solar corona than in the
photosphere. There have been observations suggesting that this observed "FIP
bias" may be different in other parts of the solar corona and such observations
are thus important in understanding the underlying mechanism. The Solar X-ray
Monitor (XSM) on board the Chandrayaan-2 mission carried out spectroscopic
observations of the Sun in soft X-rays during the 2019-20 solar minimum,
considered to be the quietest solar minimum of the past century. These
observations provided a unique opportunity to study soft X-ray spectra of the
quiescent solar corona in the absence of any active regions. By modelling high
resolution broadband X-ray spectra from XSM, we estimate the temperature and
emission measure during periods of possibly the lowest solar X-ray intensity.
We find that the derived parameters remain nearly constant over time with a
temperature around 2 MK, suggesting the emission is dominated by X-ray Bright
Points (XBPs). We also obtain the abundances of Mg, Al, and Si relative to H,
and find that the FIP bias is ~2, lower than the values observed in active
regions.
