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A multiwavelength observing campaign of the T Tauri star (TTS) GM Aur wasundertaken in 2019 December that obtained Swift X-ray and NUV fluxes, HST NUVspectra, LCOGT ugri and TESS photometry, CHIRON Halpha spectra, ALMA 13CO andC18O line fluxes, and VLA 3 cm continuum fluxes taken contemporaneously overone month. The X-ray to optical observations were presented previously. Here wepresent the ALMA and VLA data and make comparisons to GM Aur's accretion andX-ray properties. We report no variability in the observed millimeter COemission. Using disk chemistry models, we show that the magnitude of thechanges 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 tolarger changes of ~25%. However, the FUV and X-ray luminosity increases mustlast at least 100 years in order to induce changes, which seems implausible inthe 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 thatchanges of less than a factor of ~3 in the accretion rates of TTSs do not leadto detectable changes in the mass-loss rate traced by the jet at centimeterwavelengths. We conclude that typically seen changes in the FUV and X-rayluminosities of TTSs do not lead to observable changes in millimeter CO lineemission or jet centimeter continuum emission.

Testing the Potential for Radio Variability in Disks around T Tauri Stars with Observations and Chemical Modeling