The whole earth telescope - A new astronomical instrument

Nather, R. E.; Winget, D. E.; Clemens, J. C.; Hansen, Christopher J.; Hine, Butler

doi:10.1086/169196

Cited by 300 publications

(225 citation statements)

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“…More than a decade after the outstanding successes with PG 1159 and GD 358 (Winget et al 1991(Winget et al , 1994, the Whole Earth Telescope (WET; Nather et al 1990) continues to look for variable white dwarfs with rich pulsation spectra. Unfortunately we have learned that these stars are truly exceptional -either in the number and variety of their intrinsic variations, or in our ability (and luck) to detect so many modes.…”

Section: Introductionmentioning

confidence: 99%

The Consequences of Assuming m=0 for Global Model-Fitting

Metcalfe

2003

Open Astronomy

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Abstract.A recent re-analysis of Whole Earth Telescope observations of GD 358 obtained in 1990 suggest that asteroseismology of additional DBV white dwarfs can lead to independent constraints on the important, but poorly determined, 12 C(α, γ) 16 O nuclear reaction rate. Data exist for several other DBV white dwarfs, but relatively few modes are detected and there is often no multiplet structure to aid in the identification of the spherical harmonic indices l,m. I use a new grid of one million DBV models covering a broad range of masses, temperatures, and surface helium layer masses to investigate the consequences of assuming m=0 for global model-fitting. I find that when the spherical degree is known and the rotation period is of order 1 day, the model-fitting procedure applied to modes with unknown m values will still correctly identify the families of possible solutions, and has a high probability of identifying the same globally optimal solution found when the m-value is known.

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Section: Introductionmentioning

confidence: 99%

The Consequences of Assuming m=0 for Global Model-Fitting

Metcalfe

2003

Open Astronomy

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“…The Johnson V photometry was performed with the three-channel high-speed photoelectric photometer, designed for the Whole Earth Telescope campaign (Nather et al 1990;Jiang & Hu 1998) The dwarf nova, comparison and sky background were simultaneously exposed in continuous 5-s intervals. The unfiltered CCD photometry was carried out on the 60-cm telescope, which dedicated to a supernova survey.…”

Section: Photometrymentioning

confidence: 99%

A Time Evolution Study of the Superhumps of the Dwarf Nova 1RXS J232953.9+062814 by Wavelet Transform

Zhou

Qiu

2003

Astrophysics and Space Science

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Abstract. The time evolution behaviour of the superhumps of the dwarf nova 1RXS J232953.9+062814 is investigated with the wavelet analysis method. On the basis of two nights CCD photometry performed during its first superoutburst as well as other published brightness data, we reveal the superhump's time-dependence as a function of periods and time. Our light curves, which phased in the rapid decay ending portion of the superoutburst and in the dawn of a following normal outburst, are important to help trace the superhump evolution for the star. Evident amplitude variations of the superhumps, reflecting the fading of outbursts, are detected. The general profile of brightness fading over the outbursts roughly followed an exponential decay law or a form of a five-order polynomial. Both the superhump period and the orbital period of the binary system are detected in the present data. We obtain P sh =0.04575±0.00005 d and P orb =0.04496±0.00005 d. They agree with the existing values based on additional data. The two periods exchanged their roles during the superhump evolution.

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“…In order to obtain time series photometry of rapid variable stars a world-wide network of telescopes has been organised (Nather et al 1990). The network is designed to minimise or eliminate gaps in the brightness record caused by the rotation of the Earth.…”

Section: 4mentioning

confidence: 99%

Commission 9: Instruments and Techniques (Instruments et Techniques)

Davis¹

1991

Trans. Int. Astron. Union

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The period covered by this report has seen significant progress in the development of the new generation of telescopes with apertures in the 8 m plus range. The period has encompassed the major construction phase of the 10 m Keck Telescope, witnessed the commissioning of the European Southern Observatory’s (ESO) New Technology Telescope and the approval of funding for the ESO Very Large Telescope (VLT). Significant progress has been achieved in developing the necessary technology for manufacturing and figuring large mirrors. There have been major expansions of activity in the areas of active control of telescope optics and adaptive optics, and in high angular resolution interferometry with several new groups entering both fields. The use of optical fibers, particularly in the area of multiple-object spectroscopy, has continued to grow. Several telescopes can now be operated remotely and the control systems of new telescopes are being designed to facilitate remote operation.

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The whole earth telescope - A new astronomical instrument

Cited by 300 publications

References 0 publications

The Consequences of Assuming m=0 for Global Model-Fitting

The Consequences of Assuming m=0 for Global Model-Fitting

A Time Evolution Study of the Superhumps of the Dwarf Nova 1RXS J232953.9+062814 by Wavelet Transform

Commission 9: Instruments and Techniques (Instruments et Techniques)

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