Candidate objects for mid-IR variability.
|#||Name||Δtmax, corr (yr)||Δtmax, total (yr)||σrel, corr||σrel, total||Ncorr||Ntotal||Comment|
|50||EX Lup||90.4||16.5||4.9||4.9||1.5||1.1||20||17||Young eruptive star.|
|5||T Tau S||76.1||7.6||8.2||8.2||0.7||0.5||4||3||T Tauri star, a close binary system. Known IR variable (Ghez et al. 1991; Duchêne et al. 2002).|
|69||HD 150193||40.3||2.8||6.9||6.9||7.0||0.1||13||11||Herbig Ae star. Interferometric spectra are also modulated by an apparent binary signal. A comparison of ISOPHOT-S, ISO-SWS, and UKIRT/CGS3 spectra indicate significant variations both in flux level and shape of the silicate feature (Kóspál et al. 2012).|
|75||SVS20N||37.7||0.7||3.7||3.7||0.5||0.2||6||6||Embedded Herbig Ae star. A gapped model may also fit the data without the need for time variability.|
|82||HD 179218||31.7||4.4||5.3||5.3||2.0||0.1||21||6||Herbig Ae star.|
|30||V1647 Ori||30.9||2.6||0.9||0.6||0.7||0.4||9||3||Young eruptive star. MIDI observations were taken during its 20037#x2013;2006 outburst.|
|3||RY Tau||29.5||29.1||9.3||9.2||0.2||0.4||7||6||T Tauri star.|
|78||S CrA N||26.6||4.2||1.1||1.1||0.9||0.3||6||4||T Tauri star. Mid-IR variability, with an amplitude of ∼30% was also observed with Spitzer IRS and ISOPHOT-S (Kóspál et al. 2012).|
|68||V346 Nor||25.2||9.9||1.9||1.9||0.4||0.4||19||14||Young eruptive star.|
|41||CV Cha||20.7||1.0||0.8||0.8||0.4||0.2||3||3||T Tauri star. Dispersion also can be due to disk inclination. Variability was marginally observed by Kóspál et al. (2012).|
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