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tokens: the UV magnitude and flux were measured by selecting a 5-arcsec source region and a larger background region avoiding any visible sources. Flux measurements were made using the uvotmaghist software. Flux measurements from individual observations are plotted in Fig. 2 (top panel), where orange circles indicate uvw1 (2253–2946 Å) and blue diamonds are uvw2 (1599–2256 Å). They show that in both the uvw1 and uvw2 filters the first observation measured a higher flux. The following four observations all measured a slightly lower flux by about 1–2 × 10 −13 and there was no significant variability between any of the four observations from 2019 July 13 to 2019 August 10. Figure 2. Top panel: Swift UVOT flux (×10 −13 erg cm −2 s −1 ) for each observation taken over 5 weeks. Observations were made using two filters. The uvw1 filter (orange circles) and uvw2 (blue diamonds). Bottom panel: the X-ray count rate over the five observations from 2019 July 7 to 2019 August 10 in the 0.3–10 keV energy range. There is no significant change in the X-ray count rate in contrast to the decline in the UV flux. X-ray count rates were extracted from each observation using the automatic XRT data builder (Evans et al. 2007 ). The X-ray light curve in Fig. 2 , bottom panel, shows no significant variability across all the observations, including the first one where there is a higher flux in the UV. Since there is very little variation in the X-ray light curve and hardness ratio, it appears the source of the X-rays is consistent across all the observations. Therefore it is possible to combine the X-ray data to produce a single spectrum that represents the source as shown in Fig. 3 . Figure 3. The combined X-ray spectrum with a total exposure time of 10 ks. The spectrum is fitted with a two-temperature apec model without absorption. Model parameters are given in Table 3 , column 4. 3 X-RAY SPECTRAL ANALYSIS Spectral files including ancillary response file ( arf ) and response matrix file ( rmf ) were generated using the XRT automatic analysis tools (Evans et al. 2009 ) and fitting was carried out using xspec . The spectrum has relatively few photons but shows a peak at ∼1 keV and very little flux above 2 keV that are characteristics of a stellar coronal spectrum (Güdel Nazé 2009 ). We therefore fit the spectrum with an apec plasma model (Smith et al. 2001 ) as shown by the red line in Fig. 3 . The low number of counts in the spectrum requires the use of the C-statistic when fitting, rather than standard χ 2 . Single and two-temperature models were compared, with results shown in Table 3 . Fitting with a two-temperature model without absorption gave an improved fit with a reduced χ 2 of 1.27 compared to the one-temperature model’s 1.42. The temperature of the cool plasma component is 0.31 keV that is consistent with the values found for the similar K5-type T Tauri star LkCa 15 (Skinner Güdel 2013 ). However the higher temperature plasma component is almost a factor of 2