  A multiwavelength observing campaign of the T Tauri star (TTS) GM Aur was
undertaken in 2019 December that obtained Swift X-ray and NUV fluxes, HST NUV
spectra, LCOGT ugri and TESS photometry, CHIRON Halpha spectra, ALMA 13CO and
C18O line fluxes, and VLA 3 cm continuum fluxes taken contemporaneously over
one month. The X-ray to optical observations were presented previously. Here we
present the ALMA and VLA data and make comparisons to GM Aur's accretion and
X-ray properties. We report no variability in the observed millimeter CO
emission. Using disk chemistry models, we show that the magnitude of the
changes seen in the FUV luminosity of GM Aur could lead to variation of up to
~6% in CO line emission and changes in the X-ray luminosity could lead to
larger changes of ~25%. However, the FUV and X-ray luminosity increases must
last at least 100 years in order to induce changes, which seems implausible in
the TTS stage; also, these changes would be too small to be detectable by ALMA.
We report no variability in the 3 cm emission observed by the VLA, showing that
changes of less than a factor of ~3 in the accretion rates of TTSs do not lead
to detectable changes in the mass-loss rate traced by the jet at centimeter
wavelengths. We conclude that typically seen changes in the FUV and X-ray
luminosities of TTSs do not lead to observable changes in millimeter CO line
emission or jet centimeter continuum emission.
