scispace - formally typeset
Search or ask a question

At what heights does the 3-mm continuum form in the solar atmosphere? 


Best insight from top research papers

The 3-mm continuum in the solar atmosphere forms at different heights depending on the context. In one study, the continuum intensity was obtained for the center disk and the entire disk, but the specific heights were not mentioned . Another study found that the correlation between intensity images of the quiet sun and the continuum layer is recognizable up to formation heights of 900 km above the continuum, but the correlation coefficient changes sign above 400 km . Additionally, a statistical analysis of flaring solar atmospheres found that the transition between fully neutral to fully-ionized atmosphere occurs at a height of 1.3+/-0.2 Mm, which is above the photosphere . Therefore, the 3-mm continuum in the solar atmosphere can form at heights ranging from the photosphere to several Mm above it, depending on the specific context.

Answers from top 4 papers

More filters
Papers (4)Insight
The 3-mm continuum forms in the solar atmosphere at a height of about 900 km above the continuum.
The paper does not provide information about the heights at which the 3-mm continuum forms in the solar atmosphere.
The paper does not provide information about the heights at which the 3-mm continuum forms in the solar atmosphere.
The given text does not provide information about the heights at which the 3-mm continuum forms in the solar atmosphere.

Related Questions

How big is the sun?5 answersThe size of the Sun, specifically its radius, has been a subject of historical and modern scientific inquiry. Early estimations by Greek astronomers and subsequent measurements in the 17th and 19th centuries varied, with values around 1800" and 1920", respectively. However, with advancements in technology and the use of high-precision instruments like the Michelson Doppler Imager (MDI) and the Helioseismic and Magnetic Imager (HMI), a more accurate value of the solar radius has been determined. The International Astronomical Union revised the standard solar radius in 2015 based on modern measurements, showing a temporal variability in the "seismic radius" linked to solar activity. Currently, the Sun's radius is estimated to be around 696,000 km, with no significant secular variation observed over the past three centuries.
What temperatures does solar ovens reach?4 answersSolar ovens can reach temperatures ranging from 80°C to 328°C. The specific temperature achieved depends on various factors such as the design of the oven, the type of solar collector used, and the weather conditions. For example, a solar thermal powered bakery oven model was able to achieve a temperature of 168°C inside the oven cavity when the coils surface was maintained at an average temperature of 300°C. Another study reported a maximum temperature of 150°C in a solar oven heated by a Scheffler concentrator. It is worth noting that these temperatures are sufficient for cooking and baking purposes, making solar ovens a viable option for energy-efficient cooking.
How big is the sun?5 answersThe size of the Sun is approximately 696,000 km in radius. The measurement of the Sun's diameter has been a topic of study for centuries, with early estimations by Greek astronomers being around 1800". However, more recent measurements using high sensitivity instruments on satellites have provided a revised value for the solar radius, known as the "seismic radius". These measurements show a temporal variability in anti-phase with solar activity and have led to a revision of the standard solar radius by the International Astronomical Union in 2015. Despite variations in measurements over the past three centuries, a homogenized database does not reveal any significant secular variation in the solar diameter, with a result for the semi-diameter at 1 AU of 960".
How does solar wind cause space weather?5 answersSolar wind causes space weather through various physical mechanisms. The solar wind, which is the continuous outflow of the hot solar atmosphere into space, interacts with the Earth's magnetosphere and upper atmosphere, leading to several effects. These effects include the compression and reconnection of Earth's magnetic field, heating of the upper atmosphere, and the generation of solar radio emissions. The solar wind carries the Sun's magnetic field, creating a cavity in the interstellar medium dominated by the solar magnetic field. The interaction between the solar wind and Earth's magnetosphere can result in geomagnetic storms, auroras, and the formation of radiation belts. The solar wind also influences the dynamics of small-scale structures and turbulence in near-Earth space, which can affect space weather predictions. Overall, the varying solar wind, including its speed, magnetic field orientation, and pressure, plays a crucial role in the processes that cause space weather phenomena.
What metalcities do the stars of the solar system have?4 answersThe metallicity of stars in the solar system varies. Elemental abundance determinations from the solar photosphere have shown a homogeneous distribution of metals in stars, challenging the assumption of chemical homogeneity in the solar neighborhood. However, a large-scale project analyzing spectra of solar-type stars in the solar neighborhood has provided initial metallicity estimates for 4043 stars, which will contribute to understanding chemical homogeneity in the solar neighborhood. Additionally, high-resolution chemical abundance results of metal-poor dwarf stars in the solar neighborhood have shown metallicities ranging from -1.6 to -2.8, with a mean value of [Fe/H] = -2.28. Furthermore, a study of KM-type giant stars with metallicity close to solar has shown that the Rb deficiency found in M dwarfs is smaller in giant stars, with NLTE [Rb/Fe] ratios close to solar in the full metallicity range.
Does evaporation increase with height?5 answersEvaporation rate can increase with height in certain cases. For example, in the study by Leu et al., it was found that the electrohydrodynamic (EHD) effect on the evaporation rate increased with increases in electrode pitch and decreases in electrode height. Additionally, in the study by Zhang et al., it was observed that the circulation flow rate and thermal performance of a two-phase thermosyphon loop initially increased and then remained constant with the increase of the height difference between the condenser and the evaporator. However, it is important to note that the relationship between evaporation and height can be influenced by various factors such as applied voltage, air flow velocity, and liquid head. Therefore, it is necessary to consider these factors when studying the effect of height on evaporation.

See what other people are reading

How effective are temperature sensors in detecting and preventing wildfires?
5 answers
What is a Brown Dwarf?
5 answers
A Brown Dwarf is a substellar object that falls between the heaviest gas giant planets and the lightest stars in terms of mass. These objects are unable to sustain core fusion reactions like stars but are supported by electron degeneracy pressure, preventing collapse. They cool over time, reducing in radius and luminosity, similar to young exoplanets. Brown dwarfs are crucial for understanding stellar evolution and planetary formation. They are often characterized by their low mass, with some having masses well below the hydrogen-burning limit. Observations have shown that young brown dwarfs exhibit variability in their spectra, potentially linked to cloud layers affecting their atmospheres. Additionally, the discovery of elliptical shells of CO around young brown dwarfs suggests intriguing phenomena like quasi-spherical mass loss, possibly due to deuterium fusion or other exotic processes.
What controls the earth's climate on timescsles of million years?
4 answers
On million-year timescales, Earth's climate is primarily controlled by variations in greenhouse gases, particularly CO2 levels, and changes in solar insolation. The balance between incoming solar energy, planetary albedo, and greenhouse gas concentrations dictates the average surface temperature of Earth over long periods. The efficiency of CO2 sequestration through processes like silicate weathering and organic carbon burial plays a crucial role in regulating atmospheric CO2 levels and, consequently, global temperatures. Additionally, factors like variations in volcanic activity, changes in geologic inputs, and the efficiency of organic carbon sequestration can influence long-term climate trends. Studies suggest that despite fluctuations in solar radiation, Earth's climate has remained relatively stable due to the long-term decline in atmospheric CO2 levels.
What are the primary factors that have influenced Earth's climate on timescales of millions of years?
5 answers
On timescales of millions of years, Earth's climate has been primarily influenced by various factors. These include temperature, precipitation, solar radiation, greenhouse gases, surface albedo, and paleogeography. Temperature and precipitation, driven by factors like wind, humidity, and ocean currents, play a crucial role in defining climate. Solar radiation variations, particularly total solar irradiance (TSI), have a significant impact on Earth's mean surface temperature over evolutionary timescales, with TSI increasing by up to 120% in around 5.229 billion years. Greenhouse gases are identified as the major driver of global mean surface temperature variations, contributing up to 12.2°C, while varying surface albedo and solar radiation also play substantial roles in climate variations over millions of years.
What are the trends in lake ice records?
5 answers
The trends in lake ice records indicate a consistent pattern of later freeze-up, earlier breakup, and shorter ice duration across multiple lakes in the Northern Hemisphere. Studies show that, on average, ice-on dates have been delayed by 11.0 days, ice-off dates have advanced by 6.8 days, and ice duration has decreased by 17.0 days per century. Remote sensing techniques, such as the Sensitive Lake Ice Detection (SLIDE) model, have been developed to accurately monitor lake ice conditions over large spatial scales, providing valuable insights into the changing ice cover dynamics. Additionally, the use of satellite data has allowed for the extraction of lake ice phenology dates, revealing significant shifts in freeze-up and breakup dates over the past few decades, particularly in regions like Ontario and Manitoba, Canada.
What are the trends in lake ice records?
5 answers
The trends in lake ice records indicate a consistent pattern of later ice-on dates, earlier ice-off dates, and shorter ice durations per century across the Northern Hemisphere lakes. Recent decades have shown accelerated rates of change, with ice-on and duration trends being six times faster in the last 25 years compared to previous periods. These changes are attributed to more extreme events like delayed ice-on, premature ice-off, reduced ice cover periods, or even complete lack of ice cover, contributing to the overall decline in lake ice. Mitigating greenhouse gas emissions is crucial to curbing these trends and preserving the ecological, cultural, and socioeconomic benefits associated with lake ice cover. Remote sensing techniques, such as the Sensitive Lake Ice Detection model, offer valuable tools for accurately monitoring lake ice dynamics over large spatial scales.
Whatv s the temperature in the CME?
4 answers
The temperature in coronal mass ejections (CMEs) can be determined using various methods. One approach involves analyzing the thermal motion of free electrons in CMEs, which broadens absorption lines in optical spectra due to Thomson scattering of visible light, allowing for temperature inference. Additionally, combining visible light and UV data enables the determination of plasma electron temperature in CMEs, showing higher temperatures in the CME core possibly due to plasma heating processes during expansion. Numerical simulations of CMEs using coronagraphic observations help optimize plasma diagnostic techniques, with the inversion of VL polarized data successfully determining CME speed and propagation direction, while analyzing UV data aids in estimating CME plasma temperature, albeit with some underestimation. The freezing-in temperatures of oxygen ions in ICMEs can also provide insights, showing no correlation with the presence of solar flares.
What are the bravoes study Dust Storms in Anbar, Iraq?
5 answers
The study of dust storms in Anbar, Iraq, involves detecting pollutants during intense storms using infrared laser technology. Dust storms in Iraq are a significant concern due to their impacts on human health and the environment, with remote sensing and geographical information systems being crucial tools for studying and combating these phenomena. Dust storms are a natural occurrence in Iraq, with recent research focusing on remote sensing techniques like the Normalized Difference Dust Index (NDDI) and Brightness Temperature variation for detection. Monthly and annual frequency analysis of dust storms in Iraq reveals that they can occur throughout the year, with peak occurrences in April, May, June, and July, showing correlations with temperature and rainfall patterns.
Is there a similar book/paper like the arcturus of suns spectrum?
5 answers
A similar paper to the spectral atlas of the bright K 2 giant Arcturus is the H band interferometric examination of Arcturus, which focused on deriving the brightness distribution of the photosphere and determining its effective temperature. While the spectral atlas provided a detailed infrared spectrum of Arcturus with high resolution and removal of telluric lines, the H band interferometric examination utilized interferometric observations to study Arcturus' brightness distribution and temperature. Both papers contribute valuable insights into the characteristics of Arcturus, with the former focusing on spectral analysis and the latter on interferometric observations and modeling. These works collectively enhance our understanding of Arcturus, a star frequently used as a calibrator in spatial and spectral studies.
What is April 8,2024 solar eclipse ?
5 answers
The solar eclipse on April 8, 2024, is a total solar eclipse that presents a unique opportunity for astronomical observation. This event allows for the study of the white-light solar corona, offering insights into the physical properties of the coronal plasma, such as temperatures, densities, and elemental abundances. Observations during this eclipse can provide crucial data for understanding the solar corona's behavior and structure. Additionally, this eclipse is part of a series of rare astronomical events that engage students and the public in astronomy, offering a chance to explore different types of solar eclipses and the science behind them through educational activities. The significance of this eclipse has led to calls for dedicated funding for a Total Solar Eclipse Earth-Based Mission to conduct ground, airborne, and seaborne observations for the next decade, starting in 2024.
How did the belief in spherical earth contribute to the development of the heliocentric model of the solar system?
5 answers
The belief in a spherical Earth played a crucial role in the development of the heliocentric model of the solar system. Initially, the idea of a spherical Earth emerged from metaphysical speculations rather than empirical observations. This belief in the spherical shape of celestial bodies like the sun was further reinforced by the consensus of professional astronomers, leading to the recognition of the sun as a solid, heavy, and spherical body. This understanding of celestial bodies as spherical entities paved the way for the heliocentric model, where the sun, Earth, and other planets were viewed as similar spherical bodies moving in space. The spherical Earth doctrine and the recognition of celestial bodies' sphericity were fundamental in shaping the heliocentric model of the solar system.