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tokens: 20092010 with Fibre-fed, Extended Range, chelle Spectrograph (FEROS), ( R 48000) installed on the La Silla 3.6-m telescope and are in the form of flux and wavelength calibrated spectra, all pre-processed using the FEROS standard data reduction pipeline. In addition, we present two spectra ( R 60000) recorded during 2013 August with the sandiford echelle spectrograph, which is mounted on the 2.1-m telescope at the McDonald Observatory, Texas. The raw data were extracted and reduced using the standard software packages of Horne Horne ( 1986 ). All absorption-line velocities quoted in this Letter are in the heliocentric frame of reference. Every HD 183324 spectra had narrow absorption lines positioned at the bottom of a rotationally broadened, but deep, stellar Ca ii -K absorption line at 3933.7. The stellar continua were each fit with a ninth-order polynomial over the same velocity ranges in order to determine a residual intensity absorption profile for the far weaker circumstellar/interstellar Ca ii K-lines. This process has been described in detail elsewhere (Welsh Montgomery 2015 ), and the resultant eight residual intensity profile plots are shown in Fig. 1 . All eight profiles consist of two complexes of absorption lines, with one set occurring at negative velocities spanning the 40 to 10kms 1 range, and the other set spanning mostly positive velocities in the 10 to 65kms 1 range. The EW of both absorption complexes were measured over these respective velocity ranges and are listed in Table 1 . The negative velocity absorption profiles are generally characterized by a two-component structure with velocities at V 22 and 33kms 1 , although an additional weak component at V 41kms 1 is detected in the 2010 August 31 data. The values of these two main absorption velocities are close to those of the projected velocities of the Mic and Eri local interstellar gas clouds (Redfield Linsky 2008 ). This two-component absorption component has a highly variable EW that varies from 4.0 to 10.0m. Previous observations of HD 183324 in 2011 also show a similar absorption variability of this two-component structure (Welsh Montgomery 2013 ). It is unlikely that this absorption variation is due to the passage of an interstellar cloud residing between us and HD 183324, and thus it is most probably due to the addition of circumstellar gas from evaporating exocomets. Figure 1. Observations of the Ca ii 3933.7 line showing variable circumstellar absorption over the 10 to 65kms 1 velocity range. The radial velocity of the star is at 12kms 1 . Table 1. HD 183324 Ca ii absorption data. The positive velocity profiles shown in Fig. 1 are characterized by absorption components whose strength and velocity change appreciably over time. The combined EW value of this absorption component varies from 1.8 to 9.5m and has a velocity structure with variable central velocities spanning 10 to 60kms 1 . Variability of this component was also observed at a lower level (EW = 0.8 to