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Quasi-periodic X-ray Flares from the Protostar YLW15
Astrophysics · Submitted 19 Nov 1999
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim The large-scale magnetic structure and the periodicity of the flares imply that the reheating events of the same magnetic loop originate in an interaction between the star and the disk due to the differential rotation.
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The abstract, sentence by sentence
With ASCA, we have detected three X-ray flares from the Class I protostar YLW15. The flares occurred every ~20 hours and showed an exponential decay with time constant 30-60 ks. The X-ray spectra are explained by a thin thermal plasma emission. The plasma temperature shows a fast-rise and slow-decay for each flare with kT_{peak}~4-6 keV. The emission measure of the plasma shows this time profile only for the first flare, and remains almost constant during the second and third flares at the level of the tail of the first flare. The peak flare luminosities L_{X,peak} were ~5-20 * 10^{31} erg s^{-1}, which are among the brightest X-ray luminosities observed to date for Class I protostars. The total energy released in each flare was 3-6*10^{36} ergs. The first flare is well reproduced by the quasi-static cooling model, which is based on solar flares, and it suggests that the plasma cools mainly radiatively, confined by a semi-circular magnetic loop of length ~14 Ro with diameter-to-length ratio \~0.07. The two subsequent flares were consistent with the reheating of the same magnetic structure as of the first flare. The large-scale magnetic structure and the periodicity of the flares imply that the reheating events of the same magnetic loop originate in an interaction between the star and the disk due to the differential rotation.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | With ASCA, we have detected three X-ray flares from the Class I protostar YLW15. | result 0.78 | 0.97 | 0.06 | asserted 1.00 |
| s1 | The flares occurred every ~20 hours and showed an exponential decay with time constant 30-60 ks. | result 1.00 | 0.93 | 0.08 | asserted 1.00 |
| s2 | The X-ray spectra are explained by a thin thermal plasma emission. | result 0.66 | 0.83 | 0.05 | asserted 0.99 |
| s3 | The plasma temperature shows a fast-rise and slow-decay for each flare with kT_{peak}~4-6 keV. | result 1.00 | 0.91 | 0.05 | asserted 1.00 |
| s4 | The emission measure of the plasma shows this time profile only for the first flare, and remains almost constant during the second and third flares at the level of the tail of the first flare. | result 1.00 | 0.93 | 0.06 | asserted 1.00 |
| s5 | The peak flare luminosities L_{X,peak} were ~5-20 * 10^{31} erg s^{-1}, which are among the brightest X-ray luminosities observed to date for Class I protostars. | result 1.00 | 0.92 | 0.08 | asserted 1.00 |
| s6 | The total energy released in each flare was 3-6*10^{36} ergs. | result 1.00 | 0.92 | 0.04 | asserted 1.00 |
| s7 | The first flare is well reproduced by the quasi-static cooling model, which is based on solar flares, and it suggests that the plasma cools mainly radiatively, confined by a semi-circular magnetic loop of length ~14 Ro with diameter-to-length ratio \~0.07. | interpretation 0.92 | 0.86 | 0.15 | hedged possibility 0.78 |
| s8 | The two subsequent flares were consistent with the reheating of the same magnetic structure as of the first flare. | interpretation 0.66 | 0.89 | 0.11 | hedged possibility 0.95 |
| s9 | The large-scale magnetic structure and the periodicity of the flares imply that the reheating events of the same magnetic loop originate in an interaction between the star and the disk due to the differential rotation. | interpretation 1.00 | 0.79 | 0.78 | asserted 0.59 |
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The paper
Original abstract
With ASCA, we have detected three X-ray flares from the Class I protostar YLW15. The flares occurred every ~20 hours and showed an exponential decay with time constant 30-60 ks. The X-ray spectra are explained by a thin thermal plasma emission. The plasma temperature shows a fast-rise and slow-decay for each flare with kT_{peak}~4-6 keV. The emission measure of the plasma shows this time profile only for the first flare, and remains almost constant during the second and third flares at the level of the tail of the first flare. The peak flare luminosities L_{X,peak} were ~5-20 * 10^{31} erg s^{-1}, which are among the brightest X-ray luminosities observed to date for Class I protostars. The total energy released in each flare was 3-6*10^{36} ergs. The first flare is well reproduced by the quasi-static cooling model, which is based on solar flares, and it suggests that the plasma cools mainly radiatively, confined by a semi-circular magnetic loop of length ~14 Ro with diameter-to-length ratio \~0.07. The two subsequent flares were consistent with the reheating of the same magnetic structure as of the first flare. The large-scale magnetic structure and the periodicity of the flares imply that the reheating events of the same magnetic loop originate in an interaction between the star and the disk due to the differential rotation.
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