Weekly Notes from the Yohkoh Soft X-Ray Telescope

(Week 25, 1999)

Instrument Status

See the weekly operations report for details.

In the display above (click to enlarge), the colored lines show the times of SXT images that currently are on-line at ISAS. The purple lines are flare mode. The gaps will be considerably reduced when the NASA telemetry arrives and gets reformatted.

For a summary index listing of the weekly science reports, click here. Generally, these notes contain current research, or ideas related to current research in solar physics, as revealed by Yohkoh. They are done in "real time" and so they may contain (a) jargon, (b) blunders, or (c) trivialities. Of course they are not screened by referees! We are always happy when somebody writes a paper stimulated by one of these nuggets, and it happens frequently. The SXT Chief Observers (most of the authors) do not have any proprietary rights to the data or ideas presented.

Science Nugget: Yohkoh sees a beautiful arcade in the aftermath of the eruption of a giant polar crown prominence

Introduction

Polar crown prominences are usually very large in extent, of the order of 200,000 km or more in length, and are long-lived, often up to months. Since there are so few of them, and they live so long, their eruptions (marking the end of their lifes) are rare compared to eruptions of active region filaments.

Strong X-ray emission from loops formed through reconnection in the wake of an erupting polar crown filament, is also a rarity. The reason is that the Solar magnetic field near the poles is relatively weak, about 10 Gauss or less, compared to 100 to several 100 Gauss in active regions at mid-latitudes. The energy in the field scales as the square of the magnetic field strength, so active regions have typically at least 2 orders of magnitude more energy per unit volume as regions near the polar crown. A fraction of that energy, say 10%, is released during the filament eruption and the ensuing flare, and a part of that energy is emitted in Soft X-rays observed by SXT, by plasma in an arcade of postflare loops that has been heated to temperatures between 3 and 30 million Kelvin. So one can expect the X-ray emission in a crown arcade to be about 100 times less intense than in an active region.

Observations

This week we got lucky! A beautiful eruption of a polar crown filament in the the SE quadrant of the Solar disk was seen by several ground based and space based observatories. I will present here a brief chronology of the observations, and comment on the images. Do click to enlarge each of these images to appreciate their true beauty! The first image below on the left shows the giant southern polar crown filament on Sunday 13 June 1999 at 13:47 UT, observed from Big Bear Solar Observatory in southern California, in the light of H-alpha. The filament is dark on the disk, because it is in absorption, and light off the limb, in emission. Note how it makes at least a half-circle around the Solar South Pole. Now let's look in the same wavelength, about a day later, in the center image below, taken from Meudon observatory, near Paris on 14 June 1999 at 12:53 UT. A third of the filament has gone! As I will show later, there is good reason to believe it has erupted. But first let's look at an H-alpha image from Big Bear again on the right hand side, just a couple of hours later (14 June 1999 at 15:27 UT).

In just a few hours pretty much the whole filament has disappeared! Did it really erupt? Well, look at an image, below left, taken by the EIT telescope onboard the SOHO spacecraft, taken in the light of Helium II at 304 Angstrom on 14 June 1999 at 13:19 UT, nearly simultaneous with the Meudon image. The whole eastern part of the structure appears to be ripping into space, while the western part is still firmly on the Sun, as the Meudon image also shows. And that's not all! Look at what the LASCO C2 coronograph saw two hours after the EIT image (second image from the left below), on 14 June 1999 at 15:06 UT. The Solar disk is indicated by the white circle in the middle of the C2 occulting disk, which itself blocks out the light directly from the Sun up to 2 Solar radii above the limb -- so that it can better see the faint reflections from material higher up.

The filament, or at least the lasso-like magnetic structure coming from that same region, has already reached a distance of 6 Solar radii above the surface, just over 4 million km. If it has been travelling at a velocity of about 500 km/sec, which is typical for these types of eruptions, it must have taken off about 2 hours and 20 minutes before the time of this image, around 12:45 UT. That would not be inconsistent with the EIT image above, which shows the eruption in its early stages at 13:09 UT. We will be able to determine the velocity and the onset of the eruption more precisely by studying all the images from these instruments for that timeframe. Finally, the two images on the right hand side are from the LASCO C3 coronograph, which has a larger field of view than C2; the radius of the occulting disk is 3.7 Solar radii. The first image of the two was taken on 14 June 1999 at 16:18 UT, and shows clearly the Coronal Mass Ejection (CME) that is linked with the filament eruption. Unfortunately a small part of the image is obscured by the C3 support pylon, that holds the occulting disk in place. Just to prove that this CME is indeed connected to the eruptive event observed in H-alpha and by EIT, I put an earlier LASCO C3 image right next to it, on the extreme right hand side. That image was taken on 14 June 1999 at 12:42 UT, and there isno sign of a CME whatsoever yet. Note how the background stars are clearly visible, that is how well the occulting disk suppresses the direct sunlight.

SXT Observations

Now what did SXT see when this eruption was going on? Something quite different from all the others! Let's look at the time series of Yohkoh SXT images below. The first one is taken on 14 June 1999 at 13:44 UT, the second one at 15:23 UT, the third at 16:16 UT, and the fourth and last in this series at 19:44 UT. All images were made through the Aluminum Magnesium composite filter, and the first one has only half the resolution of the subsequent ones, which is why it is only a quarter of the size of the others when you click on it.

The first picture, taken at about an hour after the Meudon H-alpha image above, shows a cusped loop stretching out after the erupted filament. In the second X-ray picture, at about the time of the LASCO C2 image, a whole arcade of loops has emerged. Note that the brightness of this arcade, although it represents a flare event, is quite a bit less than that of the quiet active regions along the equator. The reason is the smallness of the magnetic field near the poles, as was explained in the introduction. While the filament eruption and CME continue the arcade slowly grows larger and higher in the third and fourth SXT image. An interesting feature, best seen in the full-size images, is the magnetic loop linking the arcade with a small active region near the Solar equator.

Interpretation

The sequence of events shown above will not shake the foundations of Solar flare theory. On the contrary, it agrees beautifully with one of the standard theories of Solar flares, the so-called CSHKP model. This model is named after a string of papers, both theoretical and observational, by Carmichael (1963), Sturrock (1968), Hirayama (1974), and Kopp & Pneumann (1980), that each contributed to what is now agreed upon by many (but not all!) Solar physicist as the standard model for eruptive flares. A key element of this model is that the eruption of the filament forces reconnection in a current sheet below it, leading to the formation and energization of an arcade of postflare loops: the arcade that SXT observes in Soft X-rays in the images above. An open question in this model is still the exact relation (causal and temporal) between the filament eruption and the accompanying CME. Rarely has such a pure and large-scale specimen of this type of event been observed. And only since very recently, with Yohkoh and SOHO together in orbit, has it been possible to cover these eruptions in so many different wavelengths simultaneously -- clearly, as demonstrated above, a prerequisite for putting together the global picture.

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June 21, 1999: Piet Martens
(martens@isass0.solar.isas.ac.jp)