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ULTRACAM observations of SDSS J170213.26+322954.1 - an eclipsing cataclysmic variable in the period gap
Astrophysics · Submitted 4 Jul 2006
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim The nature of the secondary star in SDSS J1702+3229 supports predictions that CVs with evolved secondary stars might be found accreting within the period gap.
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The abstract, sentence by sentence
We present high-speed, three-colour photometry of the eclipsing cataclysmic variable SDSS J170213.26+322954.1 (hereafter SDSS J1702+3229). This system has an orbital period of 2.4 hours, placing it within the ``period gap'' for cataclysmic variables. We determine the system parameters via a parameterized model of the eclipse fitted to the observed light curve by chi-squared minimization. We obtain a mass ratio of q = 0.215 +/- 0.015 and an orbital inclination i = 82.4 +- 0.4 degrees. The primary mass is M_w = 0.94 +/- 0.01 Msun. The secondary mass and radius are found to be Mr = 0.20 +/- 0.01 Msun and Rr = 0.243 +/- 0.013 Rsun respectively. We find a distance to the system of 440 +/- 30 pc, and an effective temperature for the secondary star of 3800 +/- 100 K (corresponding to a spectral type of M0 +/- 0.5V). Both the distance and effective temperature are consistent with previous values derived via spectroscopy of the red star. The secondary star is significantly less massive than expected for the orbital period, and significantly warmer than expected for its mass. This can be explained if the secondary star is significantly evolved: the mass and effective temperature are consistent with a secondary star that began mass transfer with a greatly reduced central hydrogen fraction. The nature of the secondary star in SDSS J1702+3229 supports predictions that CVs with evolved secondary stars might be found accreting within the period gap.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We present high-speed, three-colour photometry of the eclipsing cataclysmic variable SDSS J170213.26+322954.1 (hereafter SDSS J1702+3229). | contribution 0.98 | 0.97 | 0.03 | asserted 0.98 |
| s1 | This system has an orbital period of 2.4 hours, placing it within the ``period gap'' for cataclysmic variables. | background 0.72 | 0.25 | 0.03 | asserted 1.00 |
| s2 | We determine the system parameters via a parameterized model of the eclipse fitted to the observed light curve by chi-squared minimization. | method 1.00 | 0.96 | 0.03 | asserted 0.99 |
| s3 | We obtain a mass ratio of q = 0.215 +/- 0.015 and an orbital inclination i = 82.4 +- 0.4 degrees. | result 1.00 | 0.97 | 0.09 | asserted 1.00 |
| s4 | The primary mass is M_w = 0.94 +/- 0.01 Msun. | result 1.00 | 0.95 | 0.05 | asserted 1.00 |
| s5 | The secondary mass and radius are found to be Mr = 0.20 +/- 0.01 Msun and Rr = 0.243 +/- 0.013 Rsun respectively. | result 1.00 | 0.97 | 0.05 | asserted 1.00 |
| s6 | We find a distance to the system of 440 +/- 30 pc, and an effective temperature for the secondary star of 3800 +/- 100 K (corresponding to a spectral type of M0 +/- 0.5V). | result 1.00 | 0.96 | 0.06 | asserted 1.00 |
| s7 | Both the distance and effective temperature are consistent with previous values derived via spectroscopy of the red star. | result 0.74 | 0.28 | 0.04 | hedged possibility 0.59 |
| s8 | The secondary star is significantly less massive than expected for the orbital period, and significantly warmer than expected for its mass. | result 0.73 | 0.88 | 0.37 | asserted 1.00 |
| s9 | This can be explained if the secondary star is significantly evolved: the mass and effective temperature are consistent with a secondary star that began mass transfer with a greatly reduced central hydrogen fraction. | interpretation 1.00 | 0.33 | 0.28 | hedged possibility 0.96 |
| s10 | The nature of the secondary star in SDSS J1702+3229 supports predictions that CVs with evolved secondary stars might be found accreting within the period gap. | interpretation 1.00 | 0.29 | 0.70 | asserted 0.60 |
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The paper
Original abstract
We present high-speed, three-colour photometry of the eclipsing cataclysmic variable SDSS J170213.26+322954.1 (hereafter SDSS J1702+3229). This system has an orbital period of 2.4 hours, placing it within the ``period gap'' for cataclysmic variables. We determine the system parameters via a parameterized model of the eclipse fitted to the observed light curve by chi-squared minimization. We obtain a mass ratio of q = 0.215 +/- 0.015 and an orbital inclination i = 82.4 +- 0.4 degrees. The primary mass is M_w = 0.94 +/- 0.01 Msun. The secondary mass and radius are found to be Mr = 0.20 +/- 0.01 Msun and Rr = 0.243 +/- 0.013 Rsun respectively. We find a distance to the system of 440 +/- 30 pc, and an effective temperature for the secondary star of 3800 +/- 100 K (corresponding to a spectral type of M0 +/- 0.5V). Both the distance and effective temperature are consistent with previous values derived via spectroscopy of the red star. The secondary star is significantly less massive than expected for the orbital period, and significantly warmer than expected for its mass. This can be explained if the secondary star is significantly evolved: the mass and effective temperature are consistent with a secondary star that began mass transfer with a greatly reduced central hydrogen fraction. The nature of the secondary star in SDSS J1702+3229 supports predictions that CVs with evolved secondary stars might be found accreting within the period gap.
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