Tabetha S. Boyajian

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The bright star 55 Cancri is known to host five planets, including a transiting super-Earth. The study presented here yields directly determined values for 55 Cnc's stellar astrophysical parameters based on improved interferometry: R = 0.943 ± 0.010 R , T EFF = 5196 ± 24 K. We use isochrone fitting to determine 55 Cnc's age to be 10.2 ± 2.5 Gyr, implying a(More)
We present the results of long-baseline optical interferometry observations using the Precision Astronomical Visual Observations (PAVO) beam combiner at the Center for High Angular Resolution Astronomy (CHARA) Array to measure the angular sizes of three bright Kepler stars: θ Cygni, and both components of the binary system 16 Cygni. Supporting infrared(More)
Using the longest baselines of the CHARA Array, we have measured the angular diameter of the G5 V subdwarf Cas A, the first such determination for a halo population star. We compare this result to new diameters for the higher metallicity K0 V stars, Dra and HR 511, and find that the metal-poor star, Cas A, has an effective temperature (T eA ¼ 5297 AE 32 K),(More)
We present angular diameters of the Hyades giants, γ , δ 1 , , and θ 1 Tau from interferometric measurements with the CHARA Array. Our errors in the limb-darkened angular diameters for these stars are all less than 2%, and in combination with additional observable quantities, we determine the effective temperatures, linear radii, and absolute luminosities(More)
We present an updated spectroscopic orbit and a new visual orbit for the double-lined spectroscopic binary σ 2 Coronae Borealis based on radial velocity measurements at the Oak Ridge Observatory in Harvard, Massachusetts and interferometric visibility measurements at the CHARA Array on Mount Wilson. σ 2 CrB is composed of two Sun-like stars of roughly equal(More)
Using the longest baselines of the CHARA Array, we have measured the angular diameter of the G5 V subdwarf µ Cas A, the first such determination for a halo population star. We compare this result to new diameters for the higher metallicity K0 V stars, σ Dra and HR 511, and find that the metal-poor star, µ Cas A, has an effective temperature (T eff = 5297 ±(More)
A classical nova occurs when material accreting onto the surface of a white dwarf in a close binary system ignites in a thermonuclear runaway. Complex structures observed in the ejecta at late stages could result from interactions with the companion during the common-envelope phase. Alternatively, the explosion could be intrinsically bipolar, resulting from(More)
Metal-poor halo stars are important astrophysical laboratories that allow us to unravel details about many aspects of astrophysics, including the chemical conditions at the formation of our Galaxy, understanding the processes of diffusion in stellar interiors, and determining precise effective temperatures and calibration of colour-effective temperature(More)
We present the results from an optical spectroscopic analysis of the massive stars HD 37366 and HD 54662. We find that HD 37366 is a double-lined spectroscopic binary with a period of 31:8187 AE 0:0004 days, and HD 54662 is also a double-lined binary with a much longer period of 557:8 AE 0:3 days. The primary of HD 37366 is classified as O9.5 V, and it(More)