Boyajian, T.S.; LaCourse, D.M.; Rappaport, S.A.; Fabrycky, D.; Fischer, D.A.; Gandolfi, D.; Kennedy, G.M.; Liu, M.C.; Moor, A.; Olah, K.; Vida, K.; Wyatt, M.C.; Best, W.M.J.; Ciesla, F.; Csak, B.; Dupuy, T.J.; Handler, G.; Heng, K.; Korhonen, H.; Kovacs, J.; Kozakis, T.; Kriskovics, L.; Schmitt, J.R.; Szabo, Gy.; Szabo, R.; Wang, J.; Goodman, S.; Hoekstra, A.; Jek, K.J. (11 de septiembre de 2015). «Planet Hunters X. KIC 8462852- Where's the flux?»(PDF). MNRAS. Consultado el 13 de octubre de 2015.
Schaefer, Bradley E. (13 de enero de 2016). «KIC 8462852 Faded at an Average Rate of 0.165+-0.013 Magnitudes Per Century From 1890 To 1989». arXiv:1601.03256 [astro-ph.SR].
Hippke, Michael; Angerhausen, Daniel (8 de febrero de 2016). «KIC 8462852 did likely not fade during the last 100 years». arXiv:1601.07314v2 [astro-ph.EP].
Ballesteros, Fernando J.; Arnalte-Mur, Pablo; Fernandez-Soto, Alberto; Martinez, Vicent J. (23 de mayo de 2017). «KIC 8462852: Will the Trojans return in 2021?». arXiv:1705.08427 [astro-ph.EP].
Harp, G. R.; Richards, Jon; Shostak, Seth; Tarter, J. C.; Vakoch, Douglas A.; Munson, Chris (July 2016). «Radio SETI Observations of the Anomalous Star KIC 8462852». The Astrophysical Journal825 (2). 155. Bibcode:2016ApJ...825..155H. arXiv:1511.01606. doi:10.3847/0004-637X/825/2/155.
Gary, Bruce L. (4 de octubre de 2017). «Hereford Arizona Observatory photometry observations of KIC 8462852 between 2 May and 4 October 2017». BruceGary.net. Archivado desde el original el 4 de octubre de 2017. Consultado el 4 de octubre de 2017. "Note: g′-band and r′-band dip depths (and shapes) may differ, with g′-band being more sensitive to dust cloud scattering due to its shorter wavelength (0.47 vs. 0.62 micron). For a reasonable particle size distribution (e.g., Hanson, 0.2 micron) the extinction cross section ratio would produce a depth at r′-band that is 0.57 x depth at g′-band. If g′-band depth is 0.3%, for example, depth at r′-band could be 0.17%. The "Tabby Team" measurements (Fig. 3) at r′-band are compatible with that small dip depth. Incidentally, none of these shapes resemble exo-comet tail transits (as described by Rappaport et al., 2017 (link)); so the mystery of what's producing these week-timescale dips continues! Actually, long oval shapes are known to produce V-shaped dips (think of rings with a high inclination)." - bg
Gary, Bruce L. (4 de octubre de 2017). «Hereford Arizona Observatory photometry observations of KIC 8462852 between 2 May and 4 October 2017». BruceGary.net. Archivado desde el original el 4 de octubre de 2017. Consultado el 4 de octubre de 2017. "Note: g′-band and r′-band dip depths (and shapes) may differ, with g′-band being more sensitive to dust cloud scattering due to its shorter wavelength (0.47 vs. 0.62 micron). For a reasonable particle size distribution (e.g., Hanson, 0.2 micron) the extinction cross section ratio would produce a depth at r′-band that is 0.57 x depth at g′-band. If g′-band depth is 0.3%, for example, depth at r′-band could be 0.17%. The "Tabby Team" measurements (Fig. 3) at r′-band are compatible with that small dip depth. Incidentally, none of these shapes resemble exo-comet tail transits (as described by Rappaport et al., 2017 (link)); so the mystery of what's producing these week-timescale dips continues! Actually, long oval shapes are known to produce V-shaped dips (think of rings with a high inclination)." - bg
Sheikh, Mohammed A.; Weaver, Richard L.; Dahmen, Karin A. (19 de diciembre de 2016). «Avalanche Statistics Identify Intrinsic Stellar Processes near Criticality in KIC 8462852». Physical Review Letters (American Physical Society) 117 (26). 261101. Bibcode:2016PhRvL.117z1101S. doi:10.1103/PhysRevLett.117.261101.
Harp, G. R.; Richards, Jon; Shostak, Seth; Tarter, J. C.; Vakoch, Douglas A.; Munson, Chris (July 2016). «Radio SETI Observations of the Anomalous Star KIC 8462852». The Astrophysical Journal825 (2). 155. Bibcode:2016ApJ...825..155H. arXiv:1511.01606. doi:10.3847/0004-637X/825/2/155.
Sheikh, Mohammed A.; Weaver, Richard L.; Dahmen, Karin A. (19 de diciembre de 2016). «Avalanche Statistics Identify Intrinsic Stellar Processes near Criticality in KIC 8462852». Physical Review Letters (American Physical Society) 117 (26). 261101. Bibcode:2016PhRvL.117z1101S. doi:10.1103/PhysRevLett.117.261101.
Harp, G. R.; Richards, Jon; Shostak, Seth; Tarter, J. C.; Vakoch, Douglas A.; Munson, Chris (July 2016). «Radio SETI Observations of the Anomalous Star KIC 8462852». The Astrophysical Journal825 (2). 155. Bibcode:2016ApJ...825..155H. arXiv:1511.01606. doi:10.3847/0004-637X/825/2/155.
Wright, Jason (15 de octubre de 2015). «KIC 8462852: Where's the Flux?». AstroWright. Pennsylvania State University. Consultado el 16 de octubre de 2015.
Gary, Bruce L. (4 de octubre de 2017). «Hereford Arizona Observatory photometry observations of KIC 8462852 between 2 May and 4 October 2017». BruceGary.net. Archivado desde el original el 4 de octubre de 2017. Consultado el 4 de octubre de 2017. "Note: g′-band and r′-band dip depths (and shapes) may differ, with g′-band being more sensitive to dust cloud scattering due to its shorter wavelength (0.47 vs. 0.62 micron). For a reasonable particle size distribution (e.g., Hanson, 0.2 micron) the extinction cross section ratio would produce a depth at r′-band that is 0.57 x depth at g′-band. If g′-band depth is 0.3%, for example, depth at r′-band could be 0.17%. The "Tabby Team" measurements (Fig. 3) at r′-band are compatible with that small dip depth. Incidentally, none of these shapes resemble exo-comet tail transits (as described by Rappaport et al., 2017 (link)); so the mystery of what's producing these week-timescale dips continues! Actually, long oval shapes are known to produce V-shaped dips (think of rings with a high inclination)." - bg
