en:hf_data
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====== HF Data Analysis ====== | ====== HF Data Analysis ====== | ||
**What is supplied by the supplemental HF measurement? | **What is supplied by the supplemental HF measurement? | ||
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The VLF measurement gives us the basic paramteres of the upper D ionospheric layer. Within the digisonde measurement, | The VLF measurement gives us the basic paramteres of the upper D ionospheric layer. Within the digisonde measurement, | ||
- | The appropriate machine used to the HF measurement is a very small radio telescope. Our construction is similar to the ones which have earlier been used within the NASA Radio Jove Project, see http:// | + | The appropriate machine used to the HF measurement is a magnetometer, |
[[https:// | [[https:// | ||
{{: | {{: | ||
Originally, such a gadget was projected to measure the magnetic field' | Originally, such a gadget was projected to measure the magnetic field' | ||
- | However, | + | However, |
+ | The radio signal intensity level was drawn into a plot which is shown in Figure 2. It can be deduced that we can describe the dependency by an oscillation function while the relative amplitude of strong peaks is significantly differed from the basic state. \\ | ||
+ | [[https:// | ||
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+ | Using the approximation for a homogenous transmitter, | ||
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+ | By the time the energy is known, it is possible to put together the system of differential equation describing the linear momentum and the angular momentum. With these parameters, we can compute the distance where the X-ray came from. In other words, we could have computed the distance between the Earth and the infant star. \\ | ||
+ | The graph is given in Figure 4. We can see that the hypothetic distance growths rapidly with the time, but the single peaks corresponding to the outbursts approach each other well. \\ | ||
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+ | By the time these data were compared with the VLF measurement, | ||
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+ | Applying the Wien's Displacement Law, it is possible to model the emission wavelengths and reconstruct the emission spectrum, which was drawn into a graph shown in Figure 6. We could say that all of the elements having the atomic number from 1 to 7 were included in measurable intensity. The spectrum and its profile matches to the young star well. \\ | ||
+ | [[https:// | ||
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+ | \\ | ||
+ | The data were prepared by Vojtěch Laitl and Jaroslav Maxa, The František Krejčí Observatory Karlovy Vary. All rights reserved. |
en/hf_data.1460401403.txt.gz · Last modified: 2016/04/11 19:03 (external edit)