Create and Import the Word document. 创建和导入Word文档。
The software can create or import a Word file and let the user edit the Word file inside the built-in Word Editor. The software saves the user Word creation file and user reading process data into a single-file VMC database. 该软件可以创建或导入Word文件让用户在内置的Word编辑器编辑Word。软件将用户创建的Word文件和创作过程中的参阅文件和网络链接数据保存到单文件VMC数据库中。
The built-in Word reader in the software provides a user experience similar to Microsoft Word when reading Word. 使用软件内置的Word阅读器阅读Word时具备与微软的Word相似的用户体验
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Built-in Word Reader Same Experience as Microsoft Word
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Edit Works编辑作品
During the creative process, you can open the built-in Word full-featured editor by clicking the Edit Word button to edit your work. 创作过程中，可以通过点击编辑Word 按钮打开内置的Word全功能编辑器来编辑作品。
Building Mode 构建中
After clicking the Edit Word button, enter Building mode. At this time, except for the Word editor, no other windows are available. If you want to give up this editing, you can click the Cancel button on the right. 点击编辑Word按钮后，进入Building模式。此时，除了Word编辑器可用外，其它窗口都不可用。如果想放弃本次编辑，可以点击右侧的取消按钮。
Full featured Word editor全功能Word编辑器
After editing, please click the Save button. After saving, the Modify button in the upper right corner will become effective again. After clicking the Modify button, the software will exit the Building state and begin processing a series of tasks after editing the Word file. Until the VMC is reloaded and the editing task is completed. 编辑完成后请点击保存按钮。保存后，右上角的修改按钮会恢复有效。点击修改按钮后，软件将退出Building状态，并开始处理编辑Word文件后的一系列工作。直至重新加载VMC后完成本次编辑任务。
Insert Ribbon Tab 插入选项卡
Animation Template Ribbon Tab. Animation Template 选项卡。
When writing, users edit the Word file in the built-in Word Editor, save and exit it. The Word file will be interpreted and rendered by the built-in Word Reader before being displayed to the user. The Word Editor's editing and display are fully compatible with Microsoft Word. But in addition to being compatible with displaying Word content, the Word Reader can also interpret, render, and display Sanwhole Web Animation Controls. The Sanwhole Web Animation Control includes a series of controls with HTML5 animation effects, such as Hover Zoom, Zoom Modal, Slideshow, Accordion, Light Box, Accordion, List Scroller, Advanced Tabs, Tree, Custom HTML Code, etc. Slides are familiar, while Custom HTML Code supports any HTML CODE. Its typical application is to display YouTube videos, BiliBili videos, or real-time website web pages in Word. These shared videos all provide an HTML code for video sharing. Each Sanwhole Web Animation Control is a small piece of Word content. When writing, it can be added to Word as needed. This Word content will not display animation effects in the built-in Word Editor or Microsoft Word. But after being explained by the built-in Word Reader, that small section of Word content will be rendered as the corresponding animation control. The final presentation to the user is Word with various animation effects.
The Animation Template tab is used to insert web animation templates into Word files. In a Word file, each web animation template is a small section of Word content containing template text and template images. Users only need to replace the template text and template images with their own content.
在写作时，用户在编辑器中编辑写作的Word文件，保存退出后。该Word文件将交由阅读器解释和渲染之后再展示给用户。编辑器的编辑和显示与微软Word完全兼容。但阅读器除了可以兼容显示Word内容外，还可以解释、渲染、显示Sanwhole网页动画控件。Sanwhole网页动画控件包含一系列具备HTML5动画效果的控件，比如: Hover Zoom, Zoom Modal, Slideshow, Accordion, Light Box, Accordion, List Scroller, Advanced Tabs, Tree, Custom Html Code etc. 幻灯片很熟悉，而自定义HTML代码（Custom Html Code）支持任何HTML CODE， 典型应用是在Word中显示YouTube视频， BiliBili视频，或是显示实时网站网页。这些分享视频都提供一段视频分享的HTML代码。每个Sanwhole网页动画控件都是一小段Word内容。在写作时可以根据需要添加到写作的Word中。这个Word在编辑器中或微软Word中不会显示动画效果。但是经阅读器解释后，那一小段Word内容将被渲染为相应的动画控件。最终呈现给用户的是具备各种动画特效的Word。
Animation Template 选项卡用于向Word文件中插入WEB动画模板。在Word文件中，每个WEB动画模板是小段包含模板文字和模板图片的Word内容。用户仅需将模板文字和模板图片替换成自己的内容即可。
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Update Word Words. 更新Word 作品。
In addition to using the built-in Word Editor, editing Word also supports external Word editors. Due to our Word Editor being fully compatible with Microsoft Word. Therefore, it is recommended to use Microsoft Word. Avoid post production difficulties caused by incomplete compatibility between some Word editors and Microsoft Word. The specific operation is to use the Export Word button to export the Word file, then use Microsoft Word for editing, and after editing is complete, use the Update Word button to complete the task of editing Word. Please note that you must exit the Microsoft Word editor before clicking the Update Word button.
编辑Word除了可以使用内置的Word编辑器外，还支持外部的Word编辑器。由于我们的Word编辑器与微软Word完全兼容。因此，建议使用微软的Word。避免一些Word编辑器与微软Word不完全兼容而带来的后期制作困扰。具体操作是，请使用导出Word按钮导出Word文件，然后使用微软的Word进行编辑，编辑完成后再使用更新Word按钮完成编辑Word的任务。请注意，在点击更新Word按钮前，必须退出微软Word编辑器。
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Attach multimedia files, link online resources and preview in built-in media player.
Vole Briefcase lets you to attach multimedia files and link online resources to each presentation page and synchronously display medias in media player while presenting. These media can be picture, audio, video, PDF, DOCX, RTF, TXT, MHTML, CHM, etc. and online resources such as YouTube video, website, etc. Both the master presentation document and the subordinate presentation document collection are indispensable in the presentation. Vole Briefcase gracefully brings them together.
Attach and preview images
Attach and preview MP4
Attach and preview PDF
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Fully Customized Collector of Multiple Resources
Vole Briefcase can also be used as a fully customized collector of multiple resources. Any local file, offline web page, any online web page, online media file, online video embedding code can be included in the Vole Briefcase. The built-in previewer can preview a variety of file types, including: Microsoft Word, Excel, PDF, RTF, SWF, MHTML, Multiple Text, Image, Audio, Video, YouTube, Vimeo, etc. You can add attribute descriptions and detailed Microsoft word content style descriptions for each collection resource.
Attach and preview Twitter
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Whether for demonstration or self-appreciation, just the right amount of rendering will make the article pleasing to the eye. Vole Briefcase provides a fully functional Word editor that allows you to write any professional document with ease. Vole Briefcase records the source of your creative inspiration at any time by adding reference files and network link annotations. It should be emphasized here that Vole Briefcases can also incorporate various web animation controls into the work to enhance its appeal.
不论是演示还是自赏，恰到好处的渲染会令文章赏心悦目。Vole Briefcase提供全功能的Word编辑器让你书写任何专业的文档都会得心应手。Vole Briefcase通过添加参阅文件和网络链接批注来随时记录你创作灵感的来源。这里还要着重讲讲， Vole Briefcase还可以在作品中加入各种Web动画控件来提高作品的吸引力。
The Sanwhole Web Animation Control includes a series of controls with HTML5 animation effects, such as Hover Zoom, Zoom Modal, Slideshow, Accordion, Light Box, Accordion, List Scroller, Advanced Tabs, Tree, Custom HTML Code, etc. Slideshow is familiar, while Custom HTML Code supports any HTML CODE. Its typical application is to display YouTube videos, BiliBili videos, or real-time website web pages.
Sanwhole网页动画控件包含一系列具备HTML5动画效果的控件，比如: Hover Zoom, Zoom Modal, Slideshow, Accordion, Light Box, Accordion, List Scroller, Advanced Tabs, Tree, Custom Html Code etc. 幻灯片很熟悉，而自定义HTML代码（Custom Html Code）支持任何HTML CODE， 典型应用是在Word中显示YouTube视频， BiliBili视频，或是显示实时网站网页。
Please see the example below. 请看下面的例子。
The transport of energy through convection is important during many stages of stellar evolution1,2, and is best studied in our Sun3 or giant evolved stars4. Features that are attributed to convection are found on the surface of massive red supergiant stars5,6,7,8. Also for lower-mass evolved stars, indications of convection are found9,10,11,12,13, but convective timescales and sizes remain poorly constrained. Models indicate that convective motions are crucial to produce strong winds that return the products of stellar nucleosynthesis into the interstellar medium14. Here we report a series of reconstructed interferometric images of the surface of the evolved giant star R Doradus. The images reveal a stellar disk with prominent small-scale features that provide the structure and motions of convection on the stellar surface. We find that the dominant structure size of the features on the stellar disk is 0.72 ± 0.05 astronomical units. We measure the velocity of the surface motions to vary between −18 and +20 km s−1, which means that the convective timescale is approximately one month. This indicates a possible difference between the convection properties of low-mass and high-mass evolved stars.
The transport of energy through convection is important during many stages of stellar evolution1,2, and is best studied in our Sun3 or giant evolved stars4. Features that are attributed to convection are found on the surface of massive red supergiant stars5,6,7,8. Also for lower-mass evolved stars, indications of convection are found9,10,11,12,13, but convective timescales and sizes remain poorly constrained. Models indicate that convective motions are crucial to produce strong winds that return the products of stellar nucleosynthesis into the interstellar medium14. Here we report a series of reconstructed interferometric images of the surface of the evolved giant star R Doradus. The images reveal a stellar disk with prominent small-scale features that provide the structure and motions of convection on the stellar surface. We find that the dominant structure size of the features on the stellar disk is 0.72 ± 0.05 astronomical units. We measure the velocity of the surface motions to vary between −18 and +20 km s−1, which means that the convective timescale is approximately one month. This indicates a possible difference between the convection properties of low-mass and high-mass evolved stars.
Detail = The stellar surface of the AGB star R Doradus.
Detail =The spatial PSD for three epochs of observations of R Doradus.
Detail = The radius and radial velocity of the stellar surface of R Doradus.
Detail = Size of the smallest granules on the surface of R Doradus.
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The transport of energy through convection is important during many stages of stellar evolution1,2, and is best studied in our Sun3 or giant evolved stars4. Features that are attributed to convection are found on the surface of massive red supergiant stars5,6,7,8. Also for lower-mass evolved stars, indications of convection are found9,10,11,12,13, but convective timescales and sizes remain poorly constrained. Models indicate that convective motions are crucial to produce strong winds that return the products of stellar nucleosynthesis into the interstellar medium14. Here we report a series of reconstructed interferometric images of the surface of the evolved giant star R Doradus. The images reveal a stellar disk with prominent small-scale features that provide the structure and motions of convection on the stellar surface. We find that the dominant structure size of the features on the stellar disk is 0.72 ± 0.05 astronomical units. We measure the velocity of the surface motions to vary between −18 and +20 km s−1, which means that the convective timescale is approximately one month. This indicates a possible difference between the convection properties of low-mass and high-mass evolved stars.
Fig.1
Detail = The stellar surface of the AGB star R Doradus.
Fig.2
Detail =The spatial PSD for three epochs of observations of R Doradus.
Fig.3
Detail = The radius and radial velocity of the stellar surface of R Doradus.
Fig.4
Detail = Size of the smallest granules on the surface of R Doradus.
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The transport of energy through convection is important during many stages of stellar evolution1,2, and is best studied in our Sun3 or giant evolved stars4. Features that are attributed to convection are found on the surface of massive red supergiant stars5,6,7,8. Also for lower-mass evolved stars, indications of convection are found9,10,11,12,13, but convective timescales and sizes remain poorly constrained. Models indicate that convective motions are crucial to produce strong winds that return the products of stellar nucleosynthesis into the interstellar medium14. Here we report a series of reconstructed interferometric images of the surface of the evolved giant star R Doradus. The images reveal a stellar disk with prominent small-scale features that provide the structure and motions of convection on the stellar surface. We find that the dominant structure size of the features on the stellar disk is 0.72 ± 0.05 astronomical units. We measure the velocity of the surface motions to vary between −18 and +20 km s−1, which means that the convective timescale is approximately one month. This indicates a possible difference between the convection properties of low-mass and high-mass evolved stars.
The transport of energy through convection is important during many stages of stellar evolution1,2, and is best studied in our Sun3 or giant evolved stars4. Features that are attributed to convection are found on the surface of massive red supergiant stars5,6,7,8. Also for lower-mass evolved stars, indications of convection are found9,10,11,12,13, but convective timescales and sizes remain poorly constrained. Models indicate that convective motions are crucial to produce strong winds that return the products of stellar nucleosynthesis into the interstellar medium14. Here we report a series of reconstructed interferometric images of the surface of the evolved giant star R Doradus. The images reveal a stellar disk with prominent small-scale features that provide the structure and motions of convection on the stellar surface. We find that the dominant structure size of the features on the stellar disk is 0.72 ± 0.05 astronomical units. We measure the velocity of the surface motions to vary between −18 and +20 km s−1, which means that the convective timescale is approximately one month. This indicates a possible difference between the convection properties of low-mass and high-mass evolved stars.
Detail = The stellar surface of the AGB star R Doradus.
Detail =The spatial PSD for three epochs of observations of R Doradus.
Detail = The radius and radial velocity of the stellar surface of R Doradus.
Detail = Size of the smallest granules on the surface of R Doradus.
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The transport of energy through convection is important during many stages of stellar evolution1,2, and is best studied in our Sun3 or giant evolved stars4. Features that are attributed to convection are found on the surface of massive red supergiant stars5,6,7,8. Also for lower-mass evolved stars, indications of convection are found9,10,11,12,13, but convective timescales and sizes remain poorly constrained. Models indicate that convective motions are crucial to produce strong winds that return the products of stellar nucleosynthesis into the interstellar medium14. Here we report a series of reconstructed interferometric images of the surface of the evolved giant star R Doradus. The images reveal a stellar disk with prominent small-scale features that provide the structure and motions of convection on the stellar surface. We find that the dominant structure size of the features on the stellar disk is 0.72 ± 0.05 astronomical units. We measure the velocity of the surface motions to vary between −18 and +20 km s−1, which means that the convective timescale is approximately one month. This indicates a possible difference between the convection properties of low-mass and high-mass evolved stars.
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The transport of energy through convection is important during many stages of stellar evolution1,2, and is best studied in our Sun3 or giant evolved stars4. Features that are attributed to convection are found on the surface of massive red supergiant stars5,6,7,8. Also for lower-mass evolved stars, indications of convection are found9,10,11,12,13, but convective timescales and sizes remain poorly constrained. Models indicate that convective motions are crucial to produce strong winds that return the products of stellar nucleosynthesis into the interstellar medium14. Here we report a series of reconstructed interferometric images of the surface of the evolved giant star R Doradus. The images reveal a stellar disk with prominent small-scale features that provide the structure and motions of convection on the stellar surface. We find that the dominant structure size of the features on the stellar disk is 0.72 ± 0.05 astronomical units. We measure the velocity of the surface motions to vary between −18 and +20 km s−1, which means that the convective timescale is approximately one month. This indicates a possible difference between the convection properties of low-mass and high-mass evolved stars.
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The transport of energy through convection is important during many stages of stellar evolution1,2, and is best studied in our Sun3 or giant evolved stars4. Features that are attributed to convection are found on the surface of massive red supergiant stars5,6,7,8. Also for lower-mass evolved stars, indications of convection are found9,10,11,12,13, but convective timescales and sizes remain poorly constrained. Models indicate that convective motions are crucial to produce strong winds that return the products of stellar nucleosynthesis into the interstellar medium14. Here we report a series of reconstructed interferometric images of the surface of the evolved giant star R Doradus. The images reveal a stellar disk with prominent small-scale features that provide the structure and motions of convection on the stellar surface. We find that the dominant structure size of the features on the stellar disk is 0.72 ± 0.05 astronomical units. We measure the velocity of the surface motions to vary between −18 and +20 km s−1, which means that the convective timescale is approximately one month. This indicates a possible difference between the convection properties of low-mass and high-mass evolved stars.
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The transport of energy through convection is important during many stages of stellar evolution1,2, and is best studied in our Sun3 or giant evolved stars4. Features that are attributed to convection are found on the surface of massive red supergiant stars5,6,7,8. Also for lower-mass evolved stars, indications of convection are found9,10,11,12,13, but convective timescales and sizes remain poorly constrained. Models indicate that convective motions are crucial to produce strong winds that return the products of stellar nucleosynthesis into the interstellar medium14. Here we report a series of reconstructed interferometric images of the surface of the evolved giant star R Doradus. The images reveal a stellar disk with prominent small-scale features that provide the structure and motions of convection on the stellar surface. We find that the dominant structure size of the features on the stellar disk is 0.72 ± 0.05 astronomical units. We measure the velocity of the surface motions to vary between −18 and +20 km s−1, which means that the convective timescale is approximately one month. This indicates a possible difference between the convection properties of low-mass and high-mass evolved stars.
The transport of energy through convection is important during many stages of stellar evolution1,2, and is best studied in our Sun3 or giant evolved stars4. Features that are attributed to convection are found on the surface of massive red supergiant stars5,6,7,8. Also for lower-mass evolved stars, indications of convection are found9,10,11,12,13, but convective timescales and sizes remain poorly constrained. Models indicate that convective motions are crucial to produce strong winds that return the products of stellar nucleosynthesis into the interstellar medium14. Here we report a series of reconstructed interferometric images of the surface of the evolved giant star R Doradus. The images reveal a stellar disk with prominent small-scale features that provide the structure and motions of convection on the stellar surface. We find that the dominant structure size of the features on the stellar disk is 0.72 ± 0.05 astronomical units. We measure the velocity of the surface motions to vary between −18 and +20 km s−1, which means that the convective timescale is approximately one month. This indicates a possible difference between the convection properties of low-mass and high-mass evolved stars.
The transport of energy through convection is important during many stages of stellar evolution1,2, and is best studied in our Sun3 or giant evolved stars4. Features that are attributed to convection are found on the surface of massive red supergiant stars5,6,7,8. Also for lower-mass evolved stars, indications of convection are found9,10,11,12,13, but convective timescales and sizes remain poorly constrained. Models indicate that convective motions are crucial to produce strong winds that return the products of stellar nucleosynthesis into the interstellar medium14. Here we report a series of reconstructed interferometric images of the surface of the evolved giant star R Doradus. The images reveal a stellar disk with prominent small-scale features that provide the structure and motions of convection on the stellar surface. We find that the dominant structure size of the features on the stellar disk is 0.72 ± 0.05 astronomical units. We measure the velocity of the surface motions to vary between −18 and +20 km s−1, which means that the convective timescale is approximately one month. This indicates a possible difference between the convection properties of low-mass and high-mass evolved stars.
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Flexible Highlight
Highlighting during a presentation can effectively capture the user's attention. When the highlight function is turned on, the selected content will be automatically highlighted by changing the background color. The highlighted background color can be changed at any time. Therefore, you can use multiple highlight colors to mark a paragraph of content. Unhighlighting is also very fast, just right-click anywhere on the highlighted content. You can also clear all highlighted marks at once by pressing the cancel button. Highlighting does not modify the file content.
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Background Images and Background Animation.
When browsing content, Vole Briefcase can add preset background images and animate them. You can set the transparency of the background image, the display width of the content, the speed of the animation, and so on. Vole Briefcase can also conveniently add user images as backgrounds.
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Multilayer Drawing Board
In addition to explaining the content of the presentation, it is often necessary to temporarily write some content or draw some pictures on the blackboard to help the audience better understand the presentation content. This paint board can be displayed or hidden at any time. Supports text input and painting. And it supports multiple layers, and each layer also supports transparency settings. The content of the drawing board can be saved. It can also be directly added to the VMC document currently being demonstrated. The drawing board supports Graphics Tablet. The below drawing is using WACOM Intuos 2 model XD-0912-U.
If you need to save the drawing to the current VMC. You can first set up the VMC Media Exchange folder and then save the drawing to that folder. The software will automatically add the folder files to the current VMC and link it to the current Heading or Comment. To setting the VMC Media Exchange folder: App->Configure->Set VMC Media Exchange folder.
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Mind Map and Flowchart
Whether it's in personal thinking or collective decision-making. A timely mind map or flowchart can make problem analysis more accurate and conclusions more correct. It can not only unify ideas, but also facilitate step by step consistency. The system provides professional mind map and flowchart drawing, which is fast and convenient. Can be saved. It can also be directly added to the current VMC demonstration.
If you need to save the drawing to the current VMC. You can first set up the VMC Media Exchange folder and then save the drawing to that folder. The software will automatically add the folder files to the current VMC and link it to the current Heading or Comment. To setting the VMC Media Exchange folder: App->Configure->Set VMC Media Exchange folder.
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