OGLE Atlas of Variable Star Light Curves
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BL Herculis stars

BL Herculis stars are type II Cepheids with the shortest pulsation periods - between 1 and about 5 days. Below we present several typical I-band light curves of BL Herculis stars arranged in order of increasing periods. All of them were collected in 2010-2012 during the OGLE-IV survey of the Galactic bulge. Note the secondary bumps, which show up on the descending branch of the shortest-period light curves, and which progress backward in phase to the ascending branch for longer periods. This phenomenon is analogous to the Hertzsprung progression in classical Cepheids. For periods of about 3 days the secondary bumps disappear. Move the mouse pointer over the image to see the designation and J2000 equatorial coordinates of the star.

OGLE-BLG-T2CEP-276, R.A.=18:02:36.72 Dec=-29:07:03.6 OGLE-BLG-T2CEP-184, R.A.=17:55:43.81 Dec=-29:44:50.2
OGLE-BLG-T2CEP-234, R.A.=17:58:54.50 Dec=-28:21:30.5 OGLE-BLG-T2CEP-231, R.A.=17:58:47.45 Dec=-29:52:36.5
V2469 Sgr = OGLE-BLG-T2CEP-247, R.A.=17:59:53.49 Dec=-28:56:37.6 OGLE-BLG-T2CEP-175, R.A.=17:54:37.99 Dec=-31:21:33.1
OGLE-BLG-T2CEP-238, R.A.=17:59:04.98 Dec=-30:05:02.2 OGLE-BLG-T2CEP-176, R.A.=17:54:55.55 Dec=-29:57:31.3
OGLE-BLG-T2CEP-149, R.A.=17:53:12.52 Dec=-31:02:17.6

Using the photometric data obtained by the OGLE survey, we were able for the first time to confirm observationally a phenomenon theoretically predicted twenty years ago by Buchler & Moskalik (1992). In the Galactic bulge we discovered two BL Herculis stars with period doubling (Smolec et al. 2012) - their light curves display regular alternations of higher and lower maxima and minima. Move the cursor over the image to see this effect.

OGLE-BLG-T2CEP-279, R.A.=18:02:56.60 Dec=-30:42:34.4

Type II Cepheids W Virginis stars

Copyright by Igor Soszynski & OGLE Team