A Possible Period for the K-Band Brightening Episodes of GX 17+2 (2009)
Bornak, Jillian, McNamara, Bernard J., Harrison, Thomas E., Rupen, Michael, Bandyopadhyay, Reba M., Wachter, Stefanie
The low-mass X-ray binary and Z source GX 17+2 undergoes infrared K-band brightening episodes of at least 3.5 mag. The source of these episodes is not known. Prior published K-band magnitudes and new...
A Possible Period for the K-band Brightening Episodes of GX 17+2 (2009)
Bornak, Jillian, McNamara, Bernard J, Harrison, Thomas E, Rupen, Michael P, Bandyopadhyay, Reba M, Wachter, Stefanie
The low mass X-ray binary and Z source GX 17+2 undergoes infrared K-band brightening episodes of at least 3.5 magnitudes. The source of these episodes is not known. Prior published K-band magnitudes...
The origin of cyclic period changes in close binaries: the case of the Algol binary WW Cygni (2002)
Zavala, Robert T., McNamara, Bernard J., Harrison, Thomas E., Galvan, Eduardo, Galvan, Javier, Jarvis, Thomas, ...
Years to decade-long cyclic orbital period changes have been observed in several classes of close binary systems including Algols, W Ursae Majoris and RS Canum Venaticorum systems, and the...
Gelino, Dawn M., Harrison, Thomas E., McNamara, Bernard J.
We have obtained infrared photometry for the soft x-ray transient GU Mus. We present J and K_s band light curves modeled with WD98, the newest version of the Wilson-Devinney light curve modeling...
Measuring the Mass of the Black Hole in GS2000+25 Using IR Ellipsoidal Variations (1999)
Leeber, Dawn M., Harrison, Thomas E., McNamara, Bernard J.
Soft X-ray Transients (SXTs) are binary systems that are believed to consist of a black hole and a normal late type dwarf star which fills its Roche Lobe. We have used GRIM II on the ARC 3.5 meter...
Harrison, Thomas E., McNamara, Bernard J., Szkody, Paula, McAurthur, Barbara J., Benedict, G. F., Klemola, Arnold R., ...
We report astrometric parallaxes for three well known dwarf novae obtained using the Fine Guidance Sensors on the Hubble Space Telescope. We found a parallax for SS Aurigae of Pi = 5.00 +/- 0.64 mas,...