Chromospheric Carbon Monoxide Formation around a Solar Pore

Stauffer, Johnathan R.; Reardon, K.; Penn, M. J.

doi:10.3847/1538-4357/ac59b0

Cited by 4 publications

(7 citation statements)

References 37 publications

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“…The very existence of a strong horizontal magnetic field in a region of cold bubbles (Fig. 3 (b) and (c)) supports the explanations of both Ayres (1981) and Stauffer et al (2022).…”

Section: Conclusion and Discussionsupporting

confidence: 75%

“…This result suggests "cold bubbles" exist with different magnetic field structures, including unipolar, bipolar, or even more complicated structures. In recent work, Stauffer et al (2022) also reported the CO "cold bubbles" observed in the region surrounding a large pore, indicating a potential role of the magnetic field in the formation of these "cold bubbles".…”

Section: Results From Cyra Observationmentioning

confidence: 89%

“…By calculating the radially averaged 3-minutes power surrounding the pore in different observational lines, they proposed that the canopy magnetic field prevents the acoustic energy from propagating upward to heat the lower chromosphere. Although there exists a little difference between the pictures of Ayres (1981) and Stauffer et al (2022), both of them emphasize the important role of horizontal magnetic field in some "cold bubbles". Similarly, "cold bubbles" near the pore are also recorded in our two days' observation.…”

Section: Conclusion and Discussionmentioning

confidence: 93%

“…It is reasonable while may need strong and low-height horizontal magnetic fields. In a recent work by Stauffer et al (2022), they found several CO "cold bubbles" that surround a large pore. By calculating the radially averaged 3-minutes power surrounding the pore in different observational lines, they proposed that the canopy magnetic field prevents the acoustic energy from propagating upward to heat the lower chromosphere.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

“…The discovery of these strong absorption lines indicates the very existence of a large amount of cool gas with a temperature that can be as low as 3700 K in the solar atmosphere (e.g., Noyes & Hall 1972;Ayres & Testerman 1981;Ayres & Brault 1990). From observations and simulation models, it is found that the formation height for these lines is in a range from the upper photosphere to the middle chromosphere (e.g., Solanki et al 1994;Uitenbroek et al 1994;Clark et al 1995;Uitenbroek 2000;Ayres 2002;Asensio Ramos et al 2003;Wedemeyer-Böhm et al 2005;Stauffer et al 2022). However, the temperature in the temperature minimum region from the classical model of solar atmosphere gives is about 4400 K based on the emissions of strong Mg II h and k lines and Ultraviolet (UV) lines (e.g., Staath & Lemaire 1995;Uitenbroek 1997;Carlsson et al 1997).…”

Section: Introductionmentioning

confidence: 99%

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Observations of pores and surrounding regions with CO 4.66 μm lines by BBSO/CYRA

Song

Bai

Yang

et al. 2023

A&A

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Context. Solar observations of carbon monoxide (CO) indicate the existence of lower-temperature gas in the lower solar chromosphere. We present an observation of pores, and quiet-Sun, and network magnetic field regions with CO 4.66 µm lines by the Cryogenic Infrared Spectrograph (CYRA) at Big Bear Solar Observatory. Aims. We used the strong CO lines at around 4.66 µm to understand the properties of the thermal structures of lower solar atmosphere in different solar features with various magnetic field strengths. Methods. Different observations with different instruments were included: CO 4.66 µm imaging spectroscopy by CYRA, Atmospheric Imaging Assembly (AIA) 1700 Å images, Helioseismic and Magnetic Imager (HMI) continuum images, line-of-sight (LOS) magnetograms, and vector magnetograms. The data from 3D radiation magnetohydrodynamic (MHD) simulation with the Bifrost code are also employed for the first time to be compared with the observation. We used the Rybicki-Hummer (RH) code to synthesize the CO line profiles in the network regions. Results. The CO 3-2 R14 line center intensity changes to be either enhanced or diminished with increasing magnetic field strength, which should be caused by different heating effects in magnetic flux tubes with different sizes. We find several "cold bubbles" in the CO 3-2 R14 line center intensity images, which can be classified into two types. One type is located in the quiet-Sun regions without magnetic fields. The other type, which has rarely been reported in the past, is near or surrounded by magnetic fields. Notably, some are located at the edge of the magnetic network. The two kinds of cold bubbles and the relationship between cold bubble intensities and network magnetic field strength are both reproduced by the 3D MHD simulation with the Bifrost and RH codes. The simulation also shows that there is a cold plasma blob near the network magnetic fields, causing the observed cold bubbles seen in the CO 3-2 R14 line center image. Conclusions. Our observation and simulation illustrate that the magnetic field plays a vital role in the generation of some CO cold bubbles.

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“…The very existence of a strong horizontal magnetic field in a region of cold bubbles (Fig. 3 (b) and (c)) supports the explanations of both Ayres (1981) and Stauffer et al (2022).…”

Section: Conclusion and Discussionsupporting

confidence: 75%

Section: Results From Cyra Observationmentioning

confidence: 89%

Section: Conclusion and Discussionmentioning

confidence: 93%

Section: Conclusion and Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Observations of pores and surrounding regions with CO 4.66 μm lines by BBSO/CYRA

Song

Bai

Yang

et al. 2023

A&A

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Small-scale magnetic flux emergence preceding a chain of energetic solar atmospheric events

Nóbrega-Siverio,

Cabello,

Bose

et al. 2024

A&A

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Advancements in instrumentation have revealed a multitude of small-scale extreme-ultraviolet (EUV) events in the solar atmosphere and considerable effort is currently undergoing to unravel them. Our aim is to employ high-resolution and high-sensitivity magnetograms to gain a detailed understanding of the magnetic origin of such phenomena. We used coordinated observations from the Swedish 1-m Solar Telescope (SST), the Interface Region Imaging Spectrograph ( and the Solar Dynamics Observatory ( to analyze an ephemeral magnetic flux emergence episode and the following chain of small-scale energetic events. These unique observations clearly link these phenomena together. The high-resolution (0 $) magnetograms obtained with SST/CRISP allowed us to reliably measure the magnetic field at the photosphere and to detect the emerging bipole that caused the subsequent eruptive atmospheric events. Notably, this small-scale emergence episode remains indiscernible in the lower resolution SDO/HMI magnetograms (0 $). We report the appearance of a dark bubble in related to the emerging bipole, a sign of the canonical expanding magnetic dome predicted in flux emergence simulations. Evidence of reconnection are also found, first through an Ellerman bomb and later by the launch of a surge next to a UV burst. The UV burst exhibits a weak EUV counterpart in the coronal SDO/AIA channels. By calculating the differential emission measure (DEM), its plasma is shown to reach a temperature beyond 1 MK and to have densities between the upper chromosphere and transition region. Our study showcases the importance of high-resolution magnetograms in revealing the mechanisms that trigger phenomena such as EBs, UV bursts, and surges. This could hold implications for small-scale events similar to those recently reported in the EUV using Solar Orbiter. The finding of temperatures beyond 1 MK in the UV burst plasma strongly suggests that we are examining analogous features. Therefore, we recommend caution when drawing conclusions from full-disk magnetograms that lack the necessary resolution to reveal their true magnetic origin.

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Do Hα Stokes V Profiles Probe the Chromospheric Magnetic Field? An Observational Perspective*

Mathur

Nagaraju

Joshi

et al. 2023

ApJ

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We investigated the diagnostic potential of the Stokes V profile of the Hα line to probe the chromospheric line-of-sight (LOS) magnetic field (B LOS) by comparing the B LOS inferred from the weak field approximation (WFA) with that inferred from the multiline inversions of the Caii 8542 Å, Si i 8536 Å, and Fe i 8538 Å lines using the STiC inversion code. Simultaneous spectropolarimetric observations of a pore in the Ca ii 8542 Å and Hα spectral lines obtained from the SPINOR at the Dunn Solar Telescope on 2008 December 4 are used in this study. The WFA was applied on the Stokes I and V profiles of Hα line over three wavelength ranges, viz., around line core (Δλ = ±0.35 Å), line wings (Δλ = [−1.5, −0.6], and [+0.6, +1.5] Å), and full spectral range of the line (Δλ = ± 1.5 Å) to derive the B LOS. We found the maximum B LOS strengths of ∼+800 and ∼+600 G at log τ 500 = −1 and −4.5, respectively, in the pore. The morphological map of the B LOS inferred from the Hα line core is similar to the B LOS map at log τ 500 = −4.5 inferred from multiline inversions. The B LOS map inferred from the Hα line wings and full spectral range have a similar morphological structure to the B LOS map inferred at log τ 500 = −1. The B LOS estimated from Hα using WFA is weaker by a factor of ≈0.53 than that of inferred from the multiline inversions.

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Chromospheric Carbon Monoxide Formation around a Solar Pore

Cited by 4 publications

References 37 publications

Observations of pores and surrounding regions with CO 4.66 μm lines by BBSO/CYRA

Observations of pores and surrounding regions with CO 4.66 μm lines by BBSO/CYRA

Small-scale magnetic flux emergence preceding a chain of energetic solar atmospheric events

Do Hα Stokes V Profiles Probe the Chromospheric Magnetic Field? An Observational Perspective*

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